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\n \n 2022\n \n \n (3)\n \n \n

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\n \n\n \n \n \n \n \n \n VIS-IR spectroscopy of magnesium chlorides at cryogenic temperatures.\n \n \n \n \n\n\n \n De Angelis, S.; Tosi, F.; Carli, C.; Beck, P.; Brissaud, O.; Schmitt, B.; Piccioni, G.; De Sanctis, M. C.; and Capaccioni, F.\n\n\n \n\n\n\n Icarus, 373: 114756. February 2022.\n \n\n\n\n
\n\n\n\n \n \n $\"VIS-IR$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{de_angelis_vis-ir_2022,\n\ttitle = {{VIS}-{IR} spectroscopy of magnesium chlorides at cryogenic temperatures},\n\tvolume = {373},\n\tissn = {0019-1035},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0019103521004097},\n\tdoi = {10.1016/j.icarus.2021.114756},\n\tabstract = {Chlorinated compounds have been recently identified or suggested to exist in a number of planetary bodies such as Ceres, Europa, Ganymede, Enceladus and Mars, on the basis of remote sensing and in-situ measurements as well as Earth-based telescopic observations. Sodium and magnesium-bearing chlorinated compounds with different levels of hydration have been suggested to reach the surface of these bodies through ascending flows from the interior; thus, such materials could be geochemically related to the putative presence of subsurface liquid reservoirs and could bring precious information about those layers' salty composition. Laboratory spectroscopic data of chlorinated salts carried out at temperatures representative of real planetary bodies, fundamental to correctly interpret the observational data, are currently missing or incomplete. Here we present laboratory reflectance spectra of two hydrated magnesium chlorides, namely MgCl2•2H2O and MgCl2•6H2O, measured at three different grain sizes and at twelve temperature values in the range 80÷295 K. All spectra have been measured in the visible and infrared spectral range 0.5÷4.7 μm. We examined the absorption features and related spectral parameters as a function of both temperature and grain size. These reflectance spectra, as far as the infrared range beyond 2.5 μm is concerned, are the first measured and published at cryogenic temperatures, therefore these data may prove very useful for the interpretation and modeling of remote sensing spectral data from planetary missions. In particular, this new dataset will be helpful in applying spectral unmixing models to past and future observations of some icy satellites, Mars, Ceres, and possibly other Solar System bodies.},\n\tlanguage = {en},\n\turldate = {2023-06-29},\n\tjournal = {Icarus},\n\tauthor = {De Angelis, S. and Tosi, F. and Carli, C. and Beck, P. and Brissaud, O. and Schmitt, B. and Piccioni, G. and De Sanctis, M. C. and Capaccioni, F.},\n\tmonth = feb,\n\tyear = {2022},\n\tpages = {114756},\n}\n\n

\n\n\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Physical properties of the trans-Neptunian object (38628) Huya from a multi-chord stellar occultation.\n \n \n \n \n\n\n \n Santos-Sanz, P.; Ortiz, J. L.; Sicardy, B.; Popescu, M.; Benedetti-Rossi, G.; Morales, N.; Vara-Lubiano, M.; Camargo, J. I. B.; Pereira, C. L.; Rommel, F. L.; Assafin, M.; Desmars, J.; Braga-Ribas, F.; Duffard, R.; Marques Oliveira, J.; Vieira-Martins, R.; Fernández-Valenzuela, E.; Morgado, B. E.; Acar, M.; Anghel, S.; Atalay, E.; Ateş, A.; Bakiş, H.; Bakis, V.; Eker, Z.; Erece, O.; Kaspi, S.; Kayhan, C.; Kilic, S. E.; Kilic, Y.; Manulis, I.; Nedelcu, D. A.; Niaei, M. S.; Nir, G.; Ofek, E.; Ozisik, T.; Petrescu, E.; Satir, O.; Solmaz, A.; Sonka, A.; Tekes, M.; Unsalan, O.; Yesilyaprak, C.; Anghel, R.; Berteşteanu, D.; Curelaru, L.; Danescu, C.; Dumitrescu, V.; Gherase, R.; Hudin, L.; Stoian, A.; Tercu, J. O.; Truta, R.; Turcu, V.; Vantdevara, C.; Belskaya, I.; Dementiev, T. O.; Gazeas, K.; Karampotsiou, S.; Kashuba, V.; Kiss, C.; Koshkin, N.; Kozhukhov, O. M.; Krugly, Y.; Lecacheux, J.; Pal, A.; Püsküllü, Ç.; Szakats, R.; Zhukov, V.; Bamberger, D.; Mondon, B.; Perelló, C.; Pratt, A.; Schnabel, C.; Selva, A.; Teng, J. P.; Tigani, K.; Tsamis, V.; Weber, C.; Wells, G.; Kalkan, S.; Kudak, V.; Marciniak, A.; Ogloza, W.; Özdemir, T.; Pakštiene, E.; Perig, V.; and Żejmo, M.\n\n\n \n\n\n\n Astronomy & Astrophysics, 664: A130. August 2022.\n \n\n\n\n
\n\n\n\n \n \n $\"Physical$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{santos-sanz_physical_2022,\n\ttitle = {Physical properties of the trans-{Neptunian} object (38628) {Huya} from a multi-chord stellar occultation},\n\tvolume = {664},\n\tissn = {0004-6361, 1432-0746},\n\turl = {https://www.aanda.org/10.1051/0004-6361/202141546},\n\tdoi = {10.1051/0004-6361/202141546},\n\tabstract = {Context. \n              As part of our international program aimed at obtaining accurate physical properties of trans-Neptunian objects (TNOs), we predicted a stellar occultation by the TNO (38628) Huya of the star \n              Gaia \n              DR2 4352760586390566400 ( \n              m \n              G \n              = 11.5 mag) on March 18, 2019. After an extensive observational campaign geared at obtaining the astrometric data, we updated the prediction and found it favorable to central Europe. Therefore, we mobilized half a hundred of professional and amateur astronomers in this region and the occultation was finally detected by 21 telescopes located at 18 sites in Europe and Asia. This places the Huya event among the best ever observed stellar occultation by a TNO in terms of the number of chords. \n             \n             \n              Aims. \n              The aim of our work is to determine an accurate size, shape, and geometric albedo for the TNO (38628) Huya by using the observations obtained from a multi-chord stellar occultation. We also aim to provide constraints on the density and other internal properties of this TNO. \n             \n             \n              Methods. \n              The 21 positive detections of the occultation by Huya allowed us to obtain well-separated chords which permitted us to fit an ellipse for the limb of the body at the moment of the occultation (i.e., the instantaneous limb) with kilometric accuracy. \n             \n             \n              Results. \n              The projected semi-major and minor axes of the best ellipse fit obtained using the occultation data are ( \n              a \n              ′ \n              , b \n              ′) = (217.6 ± 3.5 km, 194.1 ± 6.1 km) with a position angle for the minor axis of \n              P \n              ′ = 55.2° ± 9.1. From this fit, the projected area-equivalent diameter is 411.0 ± 7.3 km. This diameter is compatible with the equivalent diameter for Huya obtained from radiometric techniques ( \n              D \n              = 406 ± 16 km). From this instantaneous limb, we obtained the geometric albedo for Huya ( \n              p \n               \n                V \n               \n              = \n              0.079 ± 0.004) and we explored possible three-dimensional shapes and constraints to the mass density for this TNO. We did not detect the satellite of Huya through this occultation, but the presence of rings or debris around Huya was constrained using the occultation data. We also derived an upper limit for a putative Pluto-like global atmosphere of about \n              p \n              surf \n              = 10 nbar.},\n\turldate = {2023-06-29},\n\tjournal = {Astronomy \\& Astrophysics},\n\tauthor = {Santos-Sanz, P. and Ortiz, J. L. and Sicardy, B. and Popescu, M. and Benedetti-Rossi, G. and Morales, N. and Vara-Lubiano, M. and Camargo, J. I. B. and Pereira, C. L. and Rommel, F. L. and Assafin, M. and Desmars, J. and Braga-Ribas, F. and Duffard, R. and Marques Oliveira, J. and Vieira-Martins, R. and Fernández-Valenzuela, E. and Morgado, B. E. and Acar, M. and Anghel, S. and Atalay, E. and Ateş, A. and Bakiş, H. and Bakis, V. and Eker, Z. and Erece, O. and Kaspi, S. and Kayhan, C. and Kilic, S. E. and Kilic, Y. and Manulis, I. and Nedelcu, D. A. and Niaei, M. S. and Nir, G. and Ofek, E. and Ozisik, T. and Petrescu, E. and Satir, O. and Solmaz, A. and Sonka, A. and Tekes, M. and Unsalan, O. and Yesilyaprak, C. and Anghel, R. and Berteşteanu, D. and Curelaru, L. and Danescu, C. and Dumitrescu, V. and Gherase, R. and Hudin, L. and Stoian, A-M. and Tercu, J. O. and Truta, R. and Turcu, V. and Vantdevara, C. and Belskaya, I. and Dementiev, T. O. and Gazeas, K. and Karampotsiou, S. and Kashuba, V. and Kiss, Cs. and Koshkin, N. and Kozhukhov, O. M. and Krugly, Y. and Lecacheux, J. and Pal, A. and Püsküllü, Ç. and Szakats, R. and Zhukov, V. and Bamberger, D. and Mondon, B. and Perelló, C. and Pratt, A. and Schnabel, C. and Selva, A. and Teng, J. P. and Tigani, K. and Tsamis, V. and Weber, C. and Wells, G. and Kalkan, S. and Kudak, V. and Marciniak, A. and Ogloza, W. and Özdemir, T. and Pakštiene, E. and Perig, V. and Żejmo, M.},\n\tmonth = aug,\n\tyear = {2022},\n\tpages = {A130},\n}\n\n

\n\n\n

\n Context. As part of our international program aimed at obtaining accurate physical properties of trans-Neptunian objects (TNOs), we predicted a stellar occultation by the TNO (38628) Huya of the star Gaia DR2 4352760586390566400 ( m G = 11.5 mag) on March 18, 2019. After an extensive observational campaign geared at obtaining the astrometric data, we updated the prediction and found it favorable to central Europe. Therefore, we mobilized half a hundred of professional and amateur astronomers in this region and the occultation was finally detected by 21 telescopes located at 18 sites in Europe and Asia. This places the Huya event among the best ever observed stellar occultation by a TNO in terms of the number of chords. Aims. The aim of our work is to determine an accurate size, shape, and geometric albedo for the TNO (38628) Huya by using the observations obtained from a multi-chord stellar occultation. We also aim to provide constraints on the density and other internal properties of this TNO. Methods. The 21 positive detections of the occultation by Huya allowed us to obtain well-separated chords which permitted us to fit an ellipse for the limb of the body at the moment of the occultation (i.e., the instantaneous limb) with kilometric accuracy. Results. The projected semi-major and minor axes of the best ellipse fit obtained using the occultation data are ( a ′ , b ′) = (217.6 ± 3.5 km, 194.1 ± 6.1 km) with a position angle for the minor axis of P ′ = 55.2° ± 9.1. From this fit, the projected area-equivalent diameter is 411.0 ± 7.3 km. This diameter is compatible with the equivalent diameter for Huya obtained from radiometric techniques ( D = 406 ± 16 km). From this instantaneous limb, we obtained the geometric albedo for Huya ( p V = 0.079 ± 0.004) and we explored possible three-dimensional shapes and constraints to the mass density for this TNO. We did not detect the satellite of Huya through this occultation, but the presence of rings or debris around Huya was constrained using the occultation data. We also derived an upper limit for a putative Pluto-like global atmosphere of about p surf = 10 nbar.\n

\n\n\n

\n \n\n \n \n \n \n \n \n Laser ablation of ‘diamonds-in-water’ for trace element and isotopic composition analysis.\n \n \n \n \n\n\n \n Weiss, Y.; Jockusch, S.; Koornneef, J. M.; Elazar, O.; and Davies, G. R.\n\n\n \n\n\n\n Journal of Analytical Atomic Spectrometry, 37(7): 1431–1441. July 2022.\n \n\n\n\n
\n\n\n\n \n \n $\"Laser$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{weiss_laser_2022,\n\ttitle = {Laser ablation of ‘diamonds-in-water’ for trace element and isotopic composition analysis},\n\tvolume = {37},\n\tissn = {1364-5544},\n\turl = {https://pubs.rsc.org/en/content/articlelanding/2022/ja/d2ja00088a},\n\tdoi = {10.1039/D2JA00088A},\n\tabstract = {A new laser ablation technique combined with mass spectrometry measurements was applied for trace elements and radiogenic isotopic analyses of high-density fluid (HDF) microinclusion-bearing diamonds. Experiments were conducted using a frequency-doubled Nd:YAG laser (532 nm, 150 mJ per pulse, 7 ns pulse duration, 30 Hz repetition rate) in a closed ultra-clean glass cuvette filled with ultrapure water. Five diamonds were ablated for 1 hour while a single diamond was repeatedly ablated for shorter periods to produce 4 different weights of ablated material. Ablations proceeded at an average rate of 7.8 mg h−1, which is a factor of {\\textgreater}10 better than previous studies. ICPMS trace element analyses of the ablated material reveal primitive mantle normalized patterns that are similar in shape to previously analyzed microinclusion-bearing diamonds. Importantly, the new ablation technique produces enough material for quantitative analysis of all rare-earth elements (REEs), even in diamonds of low element abundance levels. The 4 duplicates of a single diamond were analyzed for their Sr, Nd, and Pb isotope compositions by TIMS using 1011 or 1013 Ω resistors. The results reveal a relationship between decreasing amounts of analyte and increasing Sr and Pb isotope ratios attributed to blank contribution. No blank influence is detected on Nd isotope ratios. Ablations of a few mg provide sufficient amount of analyte to yield comparable Sr–Nd–Pb isotope values that reflect the composition of the ablated diamond. This result also suggests that HDF microinclusions within individual diamonds are rather homogeneous in their isotopic composition.},\n\tlanguage = {en},\n\tnumber = {7},\n\turldate = {2023-06-29},\n\tjournal = {Journal of Analytical Atomic Spectrometry},\n\tauthor = {Weiss, Yaakov and Jockusch, Steffen and Koornneef, Janne M. and Elazar, Oded and Davies, Gareth R.},\n\tmonth = jul,\n\tyear = {2022},\n\tpages = {1431--1441},\n}\n\n

\n\n\n\n\n\n

\n\n

\n \n 2021\n \n \n (21)\n \n \n

\n \n \n

\n \n\n \n \n \n \n \n \n VIS-NIR/SWIR Spectral Properties of H2O Ice Depending on Particle Size and Surface Temperature.\n \n \n \n \n\n\n \n Stephan, K.; Ciarniello, M.; Poch, O.; Schmitt, B.; Haack, D.; and Raponi, A.\n\n\n \n\n\n\n Minerals, 11(12): 1328. December 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"VIS-NIR/SWIR$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{stephan_vis-nirswir_2021,\n\ttitle = {{VIS}-{NIR}/{SWIR} {Spectral} {Properties} of {H2O} {Ice} {Depending} on {Particle} {Size} and {Surface} {Temperature}},\n\tvolume = {11},\n\tcopyright = {http://creativecommons.org/licenses/by/3.0/},\n\tissn = {2075-163X},\n\turl = {https://www.mdpi.com/2075-163X/11/12/1328},\n\tdoi = {10.3390/min11121328},\n\tabstract = {Laboratory measurements were performed to study the spectral signature of H2O ice between 0.4 and 4.2 µm depending on varying temperatures between 70 and 220 K. Spectral parameters of samples with particle sizes up to {\\textasciitilde}1360 µm, particle size mixtures, and different particle shapes were analyzed. The band depth (BD) of the major H2O-ice absorptions at 1.04, 1.25, 1.5, and 2 µm offers an excellent indicator for varying particle sizes in pure H2O ice. The spectral changes due to temperature rather, but not exclusively, affect the H2O-ice absorptions located at 1.31, 1.57, and 1.65 µm and the Fresnel reflection peaks at 3.1 and 3.2 µm, which strongly weaken with increasing temperature. As the BDs of the H2O-ice absorptions at 1.31, 1.57, and 1.65 µm increase, the band centers (BCs) of the H2O-ice absorptions at 1.25 and 1.5 µm slightly shift to shorter wavelengths. However, the BCs of the strong H2O-ice absorptions can also be affected by saturation in the case of large particles. The collected spectra provide a useful spectral library for future investigations of icy satellites such as Ganymede and Callisto, the major targets of ESA’s JUICE mission.},\n\tlanguage = {en},\n\tnumber = {12},\n\turldate = {2023-06-29},\n\tjournal = {Minerals},\n\tauthor = {Stephan, Katrin and Ciarniello, Mauro and Poch, Olivier and Schmitt, Bernard and Haack, David and Raponi, Andrea},\n\tmonth = dec,\n\tyear = {2021},\n\tkeywords = {ice, icy satellites, physical properties, spectroscopy},\n\tpages = {1328},\n}\n\n

\n\n\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Detection of Microorganisms and Metabolism in Dune Sand of a Low Organic Content.\n \n \n \n \n\n\n \n Rychert, K.; Wink, L.; Blohs, M.; Kumpitsch, C.; Neumann, C.; Moissl‐Eichinger, C.; and Wielgat‐Rychert, M.\n\n\n \n\n\n\n Journal of Geophysical Research: Biogeosciences, 126(10). October 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Detection$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{rychert_detection_2021,\n\ttitle = {Detection of {Microorganisms} and {Metabolism} in {Dune} {Sand} of a {Low} {Organic} {Content}},\n\tvolume = {126},\n\tissn = {2169-8953, 2169-8961},\n\turl = {https://onlinelibrary.wiley.com/doi/10.1029/2021JG006404},\n\tdoi = {10.1029/2021JG006404},\n\tlanguage = {en},\n\tnumber = {10},\n\turldate = {2023-06-28},\n\tjournal = {Journal of Geophysical Research: Biogeosciences},\n\tauthor = {Rychert, Krzysztof and Wink, Lisa and Blohs, Marcus and Kumpitsch, Christina and Neumann, Charlotte and Moissl‐Eichinger, Christine and Wielgat‐Rychert, Magdalena},\n\tmonth = oct,\n\tyear = {2021},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n The Lunar South Pole: A Geologcial Map of the South Pole-Aitken Basin Region.\n \n \n \n \n\n\n \n Poehler, C. M.; van der Bogert, C. H.; Hiesinger, H.; Ivanov, M.; and Head, J. W.\n\n\n \n\n\n\n ,1915. March 2021.\n ADS Bibcode: 2021LPI....52.1915P\n\n\n\n
\n\n\n\n \n \n $\"The$ Paper\n \n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{poehler_lunar_2021,\n\ttitle = {The {Lunar} {South} {Pole}: {A} {Geologcial} {Map} of the {South} {Pole}-{Aitken} {Basin} {Region}},\n\tshorttitle = {The {Lunar} {South} {Pole}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2021LPI....52.1915P},\n\tabstract = {We present geologcial context for future missions and studies at the lunar south pole.},\n\turldate = {2023-06-26},\n\tauthor = {Poehler, C. M. and van der Bogert, C. H. and Hiesinger, H. and Ivanov, M. and Head, J. W.},\n\tmonth = mar,\n\tyear = {2021},\n\tnote = {ADS Bibcode: 2021LPI....52.1915P},\n\tpages = {1915},\n}\n\n

\n\n\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Transition from unclassified Ktedonobacterales to Actinobacteria during amorphous silica precipitation in a quartzite cave environment.\n \n \n \n \n\n\n \n Ghezzi, D.; Sauro, F.; Columbu, A.; Carbone, C.; Hong, P.; Vergara, F.; De Waele, J.; and Cappelletti, M.\n\n\n \n\n\n\n Scientific Reports, 11(1): 3921. February 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Transition$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{ghezzi_transition_2021,\n\ttitle = {Transition from unclassified {Ktedonobacterales} to {Actinobacteria} during amorphous silica precipitation in a quartzite cave environment},\n\tvolume = {11},\n\tcopyright = {2021 The Author(s)},\n\tissn = {2045-2322},\n\turl = {https://www.nature.com/articles/s41598-021-83416-5},\n\tdoi = {10.1038/s41598-021-83416-5},\n\tabstract = {The orthoquartzite Imawarì Yeuta cave hosts exceptional silica speleothems and represents a unique model system to study the geomicrobiology associated to silica amorphization processes under aphotic and stable physical–chemical conditions. In this study, three consecutive evolution steps in the formation of a peculiar blackish coralloid silica speleothem were studied using a combination of morphological, mineralogical/elemental and microbiological analyses. Microbial communities were characterized using Illumina sequencing of 16S rRNA gene and clone library analysis of carbon monoxide dehydrogenase (coxL) and hydrogenase (hypD) genes involved in atmospheric trace gases utilization. The first stage of the silica amorphization process was dominated by members of a still undescribed microbial lineage belonging to the Ktedonobacterales order, probably involved in the pioneering colonization of quartzitic environments. Actinobacteria of the Pseudonocardiaceae and Acidothermaceae families dominated the intermediate amorphous silica speleothem and the final coralloid silica speleothem, respectively. The atmospheric trace gases oxidizers mostly corresponded to the main bacterial taxa present in each speleothem stage. These results provide novel understanding of the microbial community structure accompanying amorphization processes and of coxL and hypD gene expression possibly driving atmospheric trace gases metabolism in dark oligotrophic caves.},\n\tlanguage = {en},\n\tnumber = {1},\n\turldate = {2021-09-08},\n\tjournal = {Scientific Reports},\n\tauthor = {Ghezzi, D. and Sauro, F. and Columbu, A. and Carbone, C. and Hong, P.-Y. and Vergara, F. and De Waele, J. and Cappelletti, M.},\n\tmonth = feb,\n\tyear = {2021},\n\tpages = {3921},\n}\n\n

\n\n\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Microbiome dynamics during the HI-SEAS IV mission, and implications for future crewed missions beyond Earth.\n \n \n \n \n\n\n \n Mahnert, A.; Verseux, C.; Schwendner, P.; Koskinen, K.; Kumpitsch, C.; Blohs, M.; Wink, L.; Brunner, D.; Goessler, T.; Billi, D.; and Moissl-Eichinger, C.\n\n\n \n\n\n\n Microbiome, 9(1): 27. January 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Microbiome$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{mahnert_microbiome_2021,\n\ttitle = {Microbiome dynamics during the {HI}-{SEAS} {IV} mission, and implications for future crewed missions beyond {Earth}},\n\tvolume = {9},\n\tissn = {2049-2618},\n\turl = {https://doi.org/10.1186/s40168-020-00959-x},\n\tdoi = {10.1186/s40168-020-00959-x},\n\tabstract = {Human health is closely interconnected with its microbiome. Resilient microbiomes in, on, and around the human body will be key for safe and successful long-term space travel. However, longitudinal dynamics of microbiomes inside confined built environments are still poorly understood. Herein, we used the Hawaii Space Exploration Analog and Simulation IV (HI-SEAS IV) mission, a 1 year-long isolation study, to investigate microbial transfer between crew and habitat, in order to understand adverse developments which may occur in a future outpost on the Moon or Mars.},\n\tnumber = {1},\n\turldate = {2021-09-08},\n\tjournal = {Microbiome},\n\tauthor = {Mahnert, Alexander and Verseux, Cyprien and Schwendner, Petra and Koskinen, Kaisa and Kumpitsch, Christina and Blohs, Marcus and Wink, Lisa and Brunner, Daniela and Goessler, Theodora and Billi, Daniela and Moissl-Eichinger, Christine},\n\tmonth = jan,\n\tyear = {2021},\n\tkeywords = {16S rRNA gene amplicons, Antimicrobial resistances, Confined built environments, HI-SEAS, Indoor microbiome, Isolation, Longitudinal, Phenotype predictions, Skin microbiome, qPCR},\n\tpages = {27},\n}\n\n

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\n \n\n \n \n \n \n \n \n Trace-elemental and multi-isotopic (Sr-Nd-Pb) discrimination of jade in the circum-Caribbean: Implications for pre-colonial inter-island exchange networks.\n \n \n \n \n\n\n \n Knaf, A. C. S.; Habiba; Shafie, T.; Koornneef, J. M.; Hertwig, A.; Cárdenas-Párraga, J.; García-Casco, A.; Harlow, G. E.; Schertl, H. -.; Maresch, W. V.; López Belando, A. J.; Hofman, C. L.; Brandes, U.; and Davies, G. R.\n\n\n \n\n\n\n Journal of Archaeological Science, 135: 105466. November 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Trace-elemental$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{knaf_trace-elemental_2021,\n\ttitle = {Trace-elemental and multi-isotopic ({Sr}-{Nd}-{Pb}) discrimination of jade in the circum-{Caribbean}: {Implications} for pre-colonial inter-island exchange networks},\n\tvolume = {135},\n\tissn = {0305-4403},\n\tshorttitle = {Trace-elemental and multi-isotopic ({Sr}-{Nd}-{Pb}) discrimination of jade in the circum-{Caribbean}},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0305440321001369},\n\tdoi = {10.1016/j.jas.2021.105466},\n\tabstract = {Dense and strong, hydrothermal-metasomatic jadeitite and jadeite-omphacite rocks were used as tools and adornments throughout the wider Caribbean since initial inhabitation. Regionally, rich sources of jadeitite and jadeite-omphacite jade are known only in Guatemala (north and south of the Motagua Fault Zone), eastern Cuba and the northern Dominican Republic, establishing that humans transported jadeitic material over vast distances. This study validates that geochemical fingerprinting is a viable provenance method for Caribbean pre-colonial jadeitic lithologies. An assemblage of 101 source rocks has been characterised for trace element and combined Sr-Nd-Pb isotope compositions. Four statistical approaches (Principal Component Analysis, t-Distributed Stochastic Neighbour Embedding, Decision Tree, and Multiclass Regression) were assessed, employing source-distinct trace element ratios. A multiclass regression technique based on trace element ratios of immobile high field strength, light to medium rare earth and fluid-mobile, large-ion-lithophile elements is shown to be most effective in discriminating the four source regions. Ninety-one \\% of the Guatemalan samples can be discriminated from the Dominican and Cuban sources using La/Th, Zr/Hf and Y/Th ratios. Jadeitic rocks cropping out in the Dominican Republic can be distinguished from Cuban jades employing Er/Yb, Nb/Ta and Ba/Rb ratios with 71\\% certainty. Furthermore, the two Guatemala sources, north and south of the Motagua Fault Zone, can be discriminated by using (among others) Zr/Hf, Ta/Th, La/Sm and Dy/Y ratios with an 89\\% success rate. This raises the possibility of determining, in detail, former trading and mobility networks between different islands and the Meso- and Central American mainland within the Greater Caribbean. The provenance technique was applied to 19 pre-colonial jade celts excavated from the Late Ceramic Age Playa Grande archaeological site in the northern Dominican Republic. Three artefacts are discriminated as derived from the Guatemalan source, indicating that, despite a source of jade within 25 km, material was traded from Guatemala. The presence of Guatemalan jade in the Playa Grande lithic assemblage provides further evidence of large scale ({\\textgreater}3000 km), regional trading and indigenous knowledge transfer networks.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Journal of Archaeological Science},\n\tauthor = {Knaf, A. C. S. and {Habiba} and Shafie, T. and Koornneef, J. M. and Hertwig, A. and Cárdenas-Párraga, J. and García-Casco, A. and Harlow, G. E. and Schertl, H. -P. and Maresch, W. V. and López Belando, A. J. and Hofman, C. L. and Brandes, U. and Davies, G. R.},\n\tmonth = nov,\n\tyear = {2021},\n\tkeywords = {Circum-Caribbean, Geochemical characterisation, Indigenous mobility networks, Jade, Provenance studies, Source discrimination, Statistical approaches},\n\tpages = {105466},\n}\n\n

\n\n\n

\n Dense and strong, hydrothermal-metasomatic jadeitite and jadeite-omphacite rocks were used as tools and adornments throughout the wider Caribbean since initial inhabitation. Regionally, rich sources of jadeitite and jadeite-omphacite jade are known only in Guatemala (north and south of the Motagua Fault Zone), eastern Cuba and the northern Dominican Republic, establishing that humans transported jadeitic material over vast distances. This study validates that geochemical fingerprinting is a viable provenance method for Caribbean pre-colonial jadeitic lithologies. An assemblage of 101 source rocks has been characterised for trace element and combined Sr-Nd-Pb isotope compositions. Four statistical approaches (Principal Component Analysis, t-Distributed Stochastic Neighbour Embedding, Decision Tree, and Multiclass Regression) were assessed, employing source-distinct trace element ratios. A multiclass regression technique based on trace element ratios of immobile high field strength, light to medium rare earth and fluid-mobile, large-ion-lithophile elements is shown to be most effective in discriminating the four source regions. Ninety-one % of the Guatemalan samples can be discriminated from the Dominican and Cuban sources using La/Th, Zr/Hf and Y/Th ratios. Jadeitic rocks cropping out in the Dominican Republic can be distinguished from Cuban jades employing Er/Yb, Nb/Ta and Ba/Rb ratios with 71% certainty. Furthermore, the two Guatemala sources, north and south of the Motagua Fault Zone, can be discriminated by using (among others) Zr/Hf, Ta/Th, La/Sm and Dy/Y ratios with an 89% success rate. This raises the possibility of determining, in detail, former trading and mobility networks between different islands and the Meso- and Central American mainland within the Greater Caribbean. The provenance technique was applied to 19 pre-colonial jade celts excavated from the Late Ceramic Age Playa Grande archaeological site in the northern Dominican Republic. Three artefacts are discriminated as derived from the Guatemalan source, indicating that, despite a source of jade within 25 km, material was traded from Guatemala. The presence of Guatemalan jade in the Playa Grande lithic assemblage provides further evidence of large scale (\\textgreater3000 km), regional trading and indigenous knowledge transfer networks.\n

\n\n\n

\n \n\n \n \n \n \n \n \n Two billion years of episodic and simultaneous websteritic and eclogitic diamond formation beneath the Orapa kimberlite cluster, Botswana.\n \n \n \n \n\n\n \n Gress, M. U.; Timmerman, S.; Chinn, I. L.; Koornneef, J. M.; Thomassot, E.; van der Valk, E. A. S.; van Zuilen, K.; Bouden, N.; and Davies, G. R.\n\n\n \n\n\n\n Contributions to Mineralogy and Petrology, 176(7): 54. June 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Two$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{gress_two_2021,\n\ttitle = {Two billion years of episodic and simultaneous websteritic and eclogitic diamond formation beneath the {Orapa} kimberlite cluster, {Botswana}},\n\tvolume = {176},\n\tissn = {1432-0967},\n\turl = {https://doi.org/10.1007/s00410-021-01802-8},\n\tdoi = {10.1007/s00410-021-01802-8},\n\tabstract = {The Sm–Nd isotope systematics and geochemistry of eclogitic, websteritic and peridotitic garnet and clinopyroxene inclusions together with characteristics of their corresponding diamond hosts are presented for the Letlhakane mine, Botswana. These data are supplemented with new inclusion data from the nearby (20–30 km) Orapa and Damtshaa mines to evaluate the nature and scale of diamond-forming processes beneath the NW part of the Kalahari Craton and to provide insight into the evolution of the deep carbon cycle. The Sm–Nd isotope compositions of the diamond inclusions indicate five well-defined, discrete eclogitic and websteritic diamond-forming events in the Orapa kimberlite cluster at 220 ± 80 Ma, 746 ± 100 Ma, 1110 ± 64 Ma, 1698 ± 280 Ma and 2341 ± 21 Ma. In addition, two poorly constrained events suggest ancient eclogitic ({\\textgreater} 2700 Ma) and recent eclogitic and websteritic diamond formation ({\\textless} 140 Ma). Together with sub-calcic garnets from two harzburgitic diamonds that have Archaean Nd mantle model ages (TCHUR) between 2.86 and 3.38 Ga, the diamonds studied here span almost the entire temporal evolution of the SCLM of the Kalahari Craton. The new data demonstrate, for the first time, that diamond formation occurs simultaneously and episodically in different parageneses, reflecting metasomatism of the compositionally heterogeneous SCLM beneath the area ({\\textasciitilde} 200 km2). Diamond formation can be directly related to major tectono-magmatic events that impacted the Kalahari Craton such as crustal accretion, continental breakup and large igneous provinces. Compositions of dated inclusions, in combination with marked variations in the carbon and nitrogen isotope compositions of the host diamonds, record mixing arrays between a minimum of three components (A: peridotitic mantle; B: eclogites dominated by mafic material; C: eclogites that include recycled sedimentary material). Diamond formation appears dominated by local fluid–rock interactions involving different protoliths in the SCLM. Redistribution of carbon during fluid–rock interactions generally masks any potential temporal changes of the deep carbon cycle.},\n\tlanguage = {en},\n\tnumber = {7},\n\turldate = {2021-09-08},\n\tjournal = {Contributions to Mineralogy and Petrology},\n\tauthor = {Gress, M. U. and Timmerman, S. and Chinn, I. L. and Koornneef, J. M. and Thomassot, E. and van der Valk, E. A. S. and van Zuilen, K. and Bouden, N. and Davies, G. R.},\n\tmonth = jun,\n\tyear = {2021},\n\tpages = {54},\n}\n\n

\n\n\n

\n The Sm–Nd isotope systematics and geochemistry of eclogitic, websteritic and peridotitic garnet and clinopyroxene inclusions together with characteristics of their corresponding diamond hosts are presented for the Letlhakane mine, Botswana. These data are supplemented with new inclusion data from the nearby (20–30 km) Orapa and Damtshaa mines to evaluate the nature and scale of diamond-forming processes beneath the NW part of the Kalahari Craton and to provide insight into the evolution of the deep carbon cycle. The Sm–Nd isotope compositions of the diamond inclusions indicate five well-defined, discrete eclogitic and websteritic diamond-forming events in the Orapa kimberlite cluster at 220 ± 80 Ma, 746 ± 100 Ma, 1110 ± 64 Ma, 1698 ± 280 Ma and 2341 ± 21 Ma. In addition, two poorly constrained events suggest ancient eclogitic (\\textgreater 2700 Ma) and recent eclogitic and websteritic diamond formation (\\textless 140 Ma). Together with sub-calcic garnets from two harzburgitic diamonds that have Archaean Nd mantle model ages (TCHUR) between 2.86 and 3.38 Ga, the diamonds studied here span almost the entire temporal evolution of the SCLM of the Kalahari Craton. The new data demonstrate, for the first time, that diamond formation occurs simultaneously and episodically in different parageneses, reflecting metasomatism of the compositionally heterogeneous SCLM beneath the area (~ 200 km2). Diamond formation can be directly related to major tectono-magmatic events that impacted the Kalahari Craton such as crustal accretion, continental breakup and large igneous provinces. Compositions of dated inclusions, in combination with marked variations in the carbon and nitrogen isotope compositions of the host diamonds, record mixing arrays between a minimum of three components (A: peridotitic mantle; B: eclogites dominated by mafic material; C: eclogites that include recycled sedimentary material). Diamond formation appears dominated by local fluid–rock interactions involving different protoliths in the SCLM. Redistribution of carbon during fluid–rock interactions generally masks any potential temporal changes of the deep carbon cycle.\n

\n\n\n

\n \n\n \n \n \n \n \n \n How to distinguish red coloring matter used in prehistoric time? The contribution of visible near-infrared diffuse reflectance spectroscopy.\n \n \n \n \n\n\n \n Chalmin, E.; Schmitt, B.; Chanteraud, C.; Kergommeaux, A. C. d.; Soufi, F.; and Salomon, H.\n\n\n \n\n\n\n Color Research & Application, 46(3): 653–673. 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"How$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{chalmin_how_2021,\n\ttitle = {How to distinguish red coloring matter used in prehistoric time? {The} contribution of visible near-infrared diffuse reflectance spectroscopy},\n\tvolume = {46},\n\tissn = {1520-6378},\n\tshorttitle = {How to distinguish red coloring matter used in prehistoric time?},\n\turl = {https://onlinelibrary.wiley.com/doi/abs/10.1002/col.22647},\n\tdoi = {10.1002/col.22647},\n\tabstract = {Although the main prehistoric color used for paintings is red, knowledge of this coloring matter often boils down to saying that it is “ochre.” However, the red coloring matter of Prehistory is numerous and may have been the subject of various preparations, mixtures, or even alterations. Understanding the use and transformation of coloring matter raises questions about the technical processes but also about the supply strategies of these ancient societies. In the case of analysis of solid archaeological remains, we can access the petrography, mineralogy and chemistry of these ferruginous rocks. But, when it is about deposited powder, the means of investigation become limited. We therefore propose to test the complementarity of spectro-radiometry, a non-invasive method that allows us to obtain a spectral signature of the material whatever its mode of preparation. From six geological reference samples chosen for their color (from red to yellow) and for their mineralogical composition, spectra in the visible and near-infrared were recorded under several experimental conditions and several modes of preparation of the matter, using two spectro-gonio radiometers. It is then possible to discriminate these different coloring matter on the basis of their spectral signature and to understand the link with their mineral composition.},\n\tlanguage = {en},\n\tnumber = {3},\n\turldate = {2021-09-08},\n\tjournal = {Color Research \\& Application},\n\tauthor = {Chalmin, Emilie and Schmitt, Bernard and Chanteraud, Claire and Kergommeaux, Aurélie Chassin de and Soufi, Fayçal and Salomon, Hélène},\n\tyear = {2021},\n\tkeywords = {diffuse reflectance, prehistory, red coloring matter, rock art, visible-infrared spectra},\n\tpages = {653--673},\n}\n\n

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\n \n\n \n \n \n \n \n \n Mesozoic to Paleoproterozoic diamond growth beneath Botswana recorded by Re-Os ages from individual eclogitic and websteritic inclusions.\n \n \n \n \n\n\n \n Gress, M. U.; Pearson, D. G.; Chinn, I. L.; Thomassot, E.; and Davies, G. R.\n\n\n \n\n\n\n Lithos, 388-389: 106058. May 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Mesozoic$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{gress_mesozoic_2021,\n\ttitle = {Mesozoic to {Paleoproterozoic} diamond growth beneath {Botswana} recorded by {Re}-{Os} ages from individual eclogitic and websteritic inclusions},\n\tvolume = {388-389},\n\tissn = {0024-4937},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0024493721000943},\n\tdoi = {10.1016/j.lithos.2021.106058},\n\tabstract = {Re-Os isotope systematics are reported from a suite of eclogitic and websteritic sulphide inclusions extracted from well-characterised diamond growth zones from the Orapa and Jwaneng kimberlite clusters. Re-Os ages (786 ± 250 Ma) are within uncertainty of previously determined Sm-Nd ages (853 ± 55 Ma), demonstrating isotopic equilibrium, at varying levels of completeness, across multiple isotopic systems in different minerals at the time of diamond formation and inclusion encapsulation. These data confirm the concept that inclusion isochron ages, when used with detailed textural/ growth zone control, reflect the timing of diamond crystallisation. Our data substantiate previous Re-Os and Sm-Nd inclusion ages of diamonds from Orapa and Jwaneng, indicating that major tectono-magmatic events formed discrete diamond populations of Paleo- ({\\textasciitilde} 2.0 to 1.7 Ga), Meso- ({\\textasciitilde} 1.2 to 1.1 Ga) and Neoproterozoic ({\\textasciitilde} 0.9 to 0.75 Ga) age. Some of these processes occurred simultaneously across the Kalahari Craton and can be traced over 100's of km illustrating the significance of diamond inclusions for monitoring continental tectonics. Inclusion ages indicating diamond formation that are younger than 300 Ma appear to be more common than previously recognised, consistent with evidence of relatively abundant, young, fluid-rich “fibrous” and polycrystalline diamonds at Jwaneng and Orapa. The increasingly widespread evidence for Mesozoic diamond-forming events in southern Africa and elsewhere appears closely linked with the kimberlite-related magmatism that affected these regions and subsequently transported diamonds to the surface. The inclusion isochron ages emphasise that diamond formation is a multi-stage and episodic process that can occur contemporaneously in disparate substrates and produce multiple diamond populations in the sub-continental lithospheric mantle.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Lithos},\n\tauthor = {Gress, Michael U. and Pearson, D. Graham and Chinn, Ingrid L. and Thomassot, Emilie and Davies, Gareth R.},\n\tmonth = may,\n\tyear = {2021},\n\tkeywords = {Carbon, Nitrogen and Sulphur isotope, Eclogite, Inclusion dating, Zimbabwe and Kaapvaal Craton},\n\tpages = {106058},\n}\n\n

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\n \n\n \n \n \n \n \n \n The impact and recovery of asteroid 2018 LA.\n \n \n \n \n\n\n \n Jenniskens, P.; Gabadirwe, M.; Yin, Q.; Proyer, A.; Moses, O.; Kohout, T.; Franchi, F.; Gibson, R. L.; Kowalski, R.; Christensen, E. J.; Gibbs, A. R.; Heinze, A.; Denneau, L.; Farnocchia, D.; Chodas, P. W.; Gray, W.; Micheli, M.; Moskovitz, N.; Onken, C. A.; Wolf, C.; Devillepoix, H. A. R.; Ye, Q.; Robertson, D. K.; Brown, P.; Lyytinen, E.; Moilanen, J.; Albers, J.; Cooper, T.; Assink, J.; Evers, L.; Lahtinen, P.; Seitshiro, L.; Laubenstein, M.; Wantlo, N.; Moleje, P.; Maritinkole, J.; Suhonen, H.; Zolensky, M. E.; Ashwal, L.; Hiroi, T.; Sears, D. W.; Sehlke, A.; Maturilli, A.; Sanborn, M. E.; Huyskens, M. H.; Dey, S.; Ziegler, K.; Busemann, H.; Riebe, M. E. I.; Meier, M. M. M.; Welten, K. C.; Caffee, M. W.; Zhou, Q.; Li, Q.; Li, X.; Liu, Y.; Tang, G.; McLain, H. L.; Dworkin, J. P.; Glavin, D. P.; Schmitt-Kopplin, P.; Sabbah, H.; Joblin, C.; Granvik, M.; Mosarwa, B.; and Botepe, K.\n\n\n \n\n\n\n Meteoritics & Planetary Science, 56(4): 844–893. 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"The$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{jenniskens_impact_2021,\n\ttitle = {The impact and recovery of asteroid 2018 {LA}},\n\tvolume = {56},\n\tissn = {1945-5100},\n\turl = {https://onlinelibrary.wiley.com/doi/abs/10.1111/maps.13653},\n\tdoi = {10.1111/maps.13653},\n\tabstract = {The June 2, 2018 impact of asteroid 2018 LA over Botswana is only the second asteroid detected in space prior to impacting over land. Here, we report on the successful recovery of meteorites. Additional astrometric data refine the approach orbit and define the spin period and shape of the asteroid. Video observations of the fireball constrain the asteroid's position in its orbit and were used to triangulate the location of the fireball's main flare over the Central Kalahari Game Reserve. Twenty-three meteorites were recovered. A consortium study of eight of these classifies Motopi Pan as an HED polymict breccia derived from howardite, cumulate and basaltic eucrite, and diogenite lithologies. Before impact, 2018 LA was a solid rock of 156 cm diameter with high bulk density 2.85 g cm−3, a relatively low albedo pV 0.25, no significant opposition effect on the asteroid brightness, and an impact kinetic energy of 0.2 kt. The orbit of 2018 LA is consistent with an origin at Vesta (or its Vestoids) and delivery into an Earth-impacting orbit via the ν6 resonance. The impact that ejected 2018 LA in an orbit toward Earth occurred 22.8 ± 3.8 Ma ago. Zircons record a concordant U-Pb age of 4563 ± 11 Ma and a consistent 207Pb/206Pb age of 4563 ± 6 Ma. A much younger Pb-Pb phosphate resetting age of 4234 ± 41 Ma was found. From this impact chronology, we discuss what is the possible source crater of Motopi Pan and the age of Vesta's Veneneia impact basin.},\n\tlanguage = {en},\n\tnumber = {4},\n\turldate = {2021-09-08},\n\tjournal = {Meteoritics \\& Planetary Science},\n\tauthor = {Jenniskens, Peter and Gabadirwe, Mohutsiwa and Yin, Qing-Zhu and Proyer, Alexander and Moses, Oliver and Kohout, Tomas and Franchi, Fulvio and Gibson, Roger L. and Kowalski, Richard and Christensen, Eric J. and Gibbs, Alex R. and Heinze, Aren and Denneau, Larry and Farnocchia, Davide and Chodas, Paul W. and Gray, William and Micheli, Marco and Moskovitz, Nick and Onken, Christopher A. and Wolf, Christian and Devillepoix, Hadrien A. R. and Ye, Quanzhi and Robertson, Darrel K. and Brown, Peter and Lyytinen, Esko and Moilanen, Jarmo and Albers, Jim and Cooper, Tim and Assink, Jelle and Evers, Läslo and Lahtinen, Panu and Seitshiro, Lesedi and Laubenstein, Matthias and Wantlo, Nggie and Moleje, Phemo and Maritinkole, Joseph and Suhonen, Heikki and Zolensky, Michael E. and Ashwal, Lewis and Hiroi, Takahiro and Sears, Derek W. and Sehlke, Alexander and Maturilli, Alessandro and Sanborn, Matthew E. and Huyskens, Magdalena H. and Dey, Supratim and Ziegler, Karen and Busemann, Henner and Riebe, My E. I. and Meier, Matthias M. M. and Welten, Kees C. and Caffee, Marc W. and Zhou, Qin and Li, Qiu-Li and Li, Xian-Hua and Liu, Yu and Tang, Guo-Qiang and McLain, Hannah L. and Dworkin, Jason P. and Glavin, Daniel P. and Schmitt-Kopplin, Philippe and Sabbah, Hassan and Joblin, Christine and Granvik, Mikael and Mosarwa, Babutsi and Botepe, Koketso},\n\tyear = {2021},\n\tpages = {844--893},\n}\n\n

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\n \n\n \n \n \n \n \n \n Surface weathering on Venus: Constraints from kinetic, spectroscopic, and geochemical data.\n \n \n \n \n\n\n \n Dyar, M. D.; Helbert, J.; Cooper, R. F.; Sklute, E. C.; Maturilli, A.; Mueller, N. T.; Kappel, D.; and Smrekar, S. E.\n\n\n \n\n\n\n Icarus, 358: 114139. April 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Surface$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{dyar_surface_2021,\n\ttitle = {Surface weathering on {Venus}: {Constraints} from kinetic, spectroscopic, and geochemical data},\n\tvolume = {358},\n\tissn = {0019-1035},\n\tshorttitle = {Surface weathering on {Venus}},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0019103520304802},\n\tdoi = {10.1016/j.icarus.2020.114139},\n\tabstract = {On Venus, understanding of surface-atmosphere interactions resulting from chemical weathering is both critically important for constraining atmospheric chemistry and relative ages of surface features and multifaceted, requiring integration of diverse perspectives and disciplines of study. This paper evaluates the issue of surface alteration on Venus using multiple lines of evidence. Surface chemistry from Venera and Vega landers is inconsistent with significant breakdown from atmospheric interactions, with {\\textless}2.0 wt\\% S or less observed. Consideration of kinetics and breakdown of basalt under Venus conditions indicates diffusion of Ca {\\textgreater} Fe {\\textgreater} Mg toward the oxidizing Venus atmosphere, favoring creation of anhydrite and carbonate-rich surfaces on basalts with minor addition of hematite. When related to Venus-analog experiments, the kinetic calculations suggest a maximum coating of {\\textasciitilde}30 μm over 500,000 years. These changes would result in a slight overall volume increase in the outermost surface materials, which in turn decreases surface rock FeO contents. Those variations can be detected from orbit because emissivity is correlated with total FeO, and the predicted magnitudes are consistent with Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) observations. Models of anhydrite and hematite coatings on basalt mixtures suggest that changes in emissivity (ε) spectra due to chemical weathering can result in ca. {\\textless}0.08 shifts in total emissivity. Such gradations are small compared to the first-order effect of bulk composition on emissivity, which can cause up to {\\textasciitilde}0.80 emissivity shifts. For all these reasons, there is at present no evidence to suggest that impenetrable coatings of either hematite (ε = 0.8) or anhydrite (ε = 0.1) are present on Venus. Orbital measurements of surface emissivity on a global scale could therefore produce not only a map of rock type and surface composition based on transition metal contents (largely FeO) (Helbert et al., 2020) but also provide local scale assessments of fresh vs. mature lava flows on the surface.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Icarus},\n\tauthor = {Dyar, M. Darby and Helbert, Jörn and Cooper, Reid F. and Sklute, Elizabeth C. and Maturilli, Alessandro and Mueller, Nils T. and Kappel, David and Smrekar, Suzanne E.},\n\tmonth = apr,\n\tyear = {2021},\n\tkeywords = {Basalt, Emissivity, Hematite, Venus, Weathering},\n\tpages = {114139},\n}\n\n

\n\n\n

\n On Venus, understanding of surface-atmosphere interactions resulting from chemical weathering is both critically important for constraining atmospheric chemistry and relative ages of surface features and multifaceted, requiring integration of diverse perspectives and disciplines of study. This paper evaluates the issue of surface alteration on Venus using multiple lines of evidence. Surface chemistry from Venera and Vega landers is inconsistent with significant breakdown from atmospheric interactions, with \\textless2.0 wt% S or less observed. Consideration of kinetics and breakdown of basalt under Venus conditions indicates diffusion of Ca \\textgreater Fe \\textgreater Mg toward the oxidizing Venus atmosphere, favoring creation of anhydrite and carbonate-rich surfaces on basalts with minor addition of hematite. When related to Venus-analog experiments, the kinetic calculations suggest a maximum coating of ~30 μm over 500,000 years. These changes would result in a slight overall volume increase in the outermost surface materials, which in turn decreases surface rock FeO contents. Those variations can be detected from orbit because emissivity is correlated with total FeO, and the predicted magnitudes are consistent with Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) observations. Models of anhydrite and hematite coatings on basalt mixtures suggest that changes in emissivity (ε) spectra due to chemical weathering can result in ca. \\textless0.08 shifts in total emissivity. Such gradations are small compared to the first-order effect of bulk composition on emissivity, which can cause up to ~0.80 emissivity shifts. For all these reasons, there is at present no evidence to suggest that impenetrable coatings of either hematite (ε = 0.8) or anhydrite (ε = 0.1) are present on Venus. Orbital measurements of surface emissivity on a global scale could therefore produce not only a map of rock type and surface composition based on transition metal contents (largely FeO) (Helbert et al., 2020) but also provide local scale assessments of fresh vs. mature lava flows on the surface.\n

\n\n\n

\n \n\n \n \n \n \n \n \n Dust devils: Characteristics of the forward motion from a Saharan survey.\n \n \n \n \n\n\n \n Franzese, G.; Silvestro, S.; Vaz, D. A.; Popa, C. I.; Cozzolino, F.; Esposito, F.; Mongelluzzo, G.; Porto, C.; and Ruggeri, A. C.\n\n\n \n\n\n\n Aeolian Research, 50: 100678. March 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Dust$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{franzese_dust_2021,\n\ttitle = {Dust devils: {Characteristics} of the forward motion from a {Saharan} survey},\n\tvolume = {50},\n\tissn = {1875-9637},\n\tshorttitle = {Dust devils},\n\turl = {https://www.sciencedirect.com/science/article/pii/S187596372100015X},\n\tdoi = {10.1016/j.aeolia.2021.100678},\n\tabstract = {Dust devils have been proposed as a tool to investigate martian near-ground wind conditions. However, further studies are needed in order to fully understand how background atmospheric conditions affect dust devil forward motion. One of the main issues is related to the lack of synchronous acquisition of the dust devils forward speed and ambient wind measurements. This work aims to present an effective methodology to retrieve the dust devil translational velocity using the horizontal wind time series acquired by a single stationary anemometer, and utilize this method to deeply investigate its relation with the ambient velocity. For this purpose, we first tested the reliability of our method using the data acquired during an intensive week-long dust devil survey, during which we deployed a meteorological station coupled with a camera in a Sahara desert site. After confirming the technique by comparing the results with the ones obtained with the camera, we applied the method to a meteorological data set of 338 dust devil events we acquired in a previous Saharan campaign. We studied the characteristics of the forward velocity, observing how it closely matches the ambient wind regime, with {\\textasciitilde}70\\% of the events lying in a range of 20° and 1 m/s from the ambient velocity measured at 4.5 m. Our results indicate how the vortex forward speed follows a vertical profile similar to the boundary layer wind, confirming the effectiveness of the dust devils monitoring for the study of the surface winds.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Aeolian Research},\n\tauthor = {Franzese, Gabriele and Silvestro, Simone and Vaz, David A. and Popa, Ciprian Ionut and Cozzolino, Fabio and Esposito, Francesca and Mongelluzzo, Giuseppe and Porto, Carmen and Ruggeri, Alan Cosimo},\n\tmonth = mar,\n\tyear = {2021},\n\tkeywords = {Boundary layer wind, Dust devils, Earth, Mars, Micrometeorology},\n\tpages = {100678},\n}\n\n

\n\n\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n A lower-than-expected saltation threshold at Martian pressure and below.\n \n \n \n \n\n\n \n Andreotti, B.; Claudin, P.; Iversen, J. J.; Merrison, J. P.; and Rasmussen, K. R.\n\n\n \n\n\n\n Proceedings of the National Academy of Sciences, 118(5). February 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"A$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{andreotti_lower-than-expected_2021,\n\ttitle = {A lower-than-expected saltation threshold at {Martian} pressure and below},\n\tvolume = {118},\n\tcopyright = {© 2021 . https://www.pnas.org/site/aboutpnas/licenses.xhtmlPublished under the PNAS license.},\n\tissn = {0027-8424, 1091-6490},\n\turl = {https://www.pnas.org/content/118/5/e2012386118},\n\tdoi = {10.1073/pnas.2012386118},\n\tabstract = {Aeolian sediment transport is observed to occur on Mars as well as other extraterrestrial environments, generating ripples and dunes as on Earth. The search for terrestrial analogs of planetary bedforms, as well as environmental simulation experiments able to reproduce their formation in planetary conditions, are powerful ways to question our understanding of geomorphological processes toward unusual environmental conditions. Here, we perform sediment transport laboratory experiments in a closed-circuit wind tunnel placed in a vacuum chamber and operated at extremely low pressures to show that Martian conditions belong to a previously unexplored saltation regime. The threshold wind speed required to initiate saltation is only quantitatively predicted by state-of-the art models up to a density ratio between grain and air of 4×105 but unexpectedly falls to much lower values for higher density ratios. In contrast, impact ripples, whose emergence is continuously observed on the granular bed over the whole pressure range investigated, display a characteristic wavelength and propagation velocity essentially independent of pressure. A comparison of these findings with existing models suggests that sediment transport at low Reynolds number but high grain-to-fluid density ratio may be dominated by collective effects associated with grain inertia in the granular collisional layer.},\n\tlanguage = {en},\n\tnumber = {5},\n\turldate = {2021-09-08},\n\tjournal = {Proceedings of the National Academy of Sciences},\n\tauthor = {Andreotti, Bruno and Claudin, Philippe and Iversen, Jens Jacob and Merrison, Jonathan P. and Rasmussen, Keld R.},\n\tmonth = feb,\n\tyear = {2021},\n\tpmid = {33509927},\n\tkeywords = {Mars, impact ripples, saltation at low pressure, sediment transport threshold},\n}\n\n

\n\n\n\n\n\n

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\n \n\n \n \n \n \n \n \n Vacuum ultraviolet photoabsorption spectroscopy of space-related ices: formation and destruction of solid carbonic acid upon 1 keV electron irradiation.\n \n \n \n \n\n\n \n Ioppolo, S.; Kaňuchová, Z.; James, R. L.; Dawes, A.; Ryabov, A.; Dezalay, J.; Jones, N. C.; Hoffmann, S. V.; Mason, N. J.; and Strazzulla, G.\n\n\n \n\n\n\n Astronomy & Astrophysics, 646: A172. February 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Vacuum$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{ioppolo_vacuum_2021,\n\ttitle = {Vacuum ultraviolet photoabsorption spectroscopy of space-related ices: formation and destruction of solid carbonic acid upon 1 {keV} electron irradiation},\n\tvolume = {646},\n\tcopyright = {© ESO 2021},\n\tissn = {0004-6361, 1432-0746},\n\tshorttitle = {Vacuum ultraviolet photoabsorption spectroscopy of space-related ices},\n\turl = {https://www.aanda.org/articles/aa/abs/2021/02/aa39184-20/aa39184-20.html},\n\tdoi = {10.1051/0004-6361/202039184},\n\tabstract = {{\\textless}i{\\textgreater}Context.{\\textless}i/{\\textgreater} Carbonic acid (H{\\textless}sub{\\textgreater}2{\\textless}sub/{\\textgreater}CO{\\textless}sub{\\textgreater}3{\\textless}sub/{\\textgreater}) is a weak acid relevant to astrobiology which, to date, remains undetected in space. Experimental work has shown that the {\\textless}i{\\textgreater}β{\\textless}i/{\\textgreater}-polymorph of H{\\textless}sub{\\textgreater}2{\\textless}sub/{\\textgreater}CO{\\textless}sub{\\textgreater}3{\\textless}sub/{\\textgreater} forms under space relevant conditions through energetic (UV photon, electron, and cosmic ray) processing of CO{\\textless}sub{\\textgreater}2{\\textless}sub/{\\textgreater}- and H{\\textless}sub{\\textgreater}2{\\textless}sub/{\\textgreater}O-rich ices. Although its {\\textless}i{\\textgreater}α{\\textless}i/{\\textgreater}-polymorph ice has been recently reassigned to the monomethyl ester of carbonic acid, a different form of H{\\textless}sub{\\textgreater}2{\\textless}sub/{\\textgreater}CO{\\textless}sub{\\textgreater}3{\\textless}sub/{\\textgreater} ice may exist and is synthesized without irradiation through surface reactions involving CO molecules and OH radicals, that is to say {\\textless}i{\\textgreater}γ{\\textless}i/{\\textgreater}-H{\\textless}sub{\\textgreater}2{\\textless}sub/{\\textgreater}CO{\\textless}sub{\\textgreater}3{\\textless}sub/{\\textgreater}.{\\textless}i{\\textgreater}Aims.{\\textless}i/{\\textgreater} We aim to provide a systematic set of vacuum ultraviolet (VUV) photoabsorption spectroscopic data of pure carbonic acid that formed and was destroyed under conditions relevant to space in support of its future identification on the surface of icy objects in the Solar System by the upcoming Jupiter ICy moons Explorer mission and on interstellar dust by the {\\textless}i{\\textgreater}James Webb{\\textless}i/{\\textgreater} Space Telescope spacecraft.{\\textless}i{\\textgreater}Methods.{\\textless}i/{\\textgreater} We present VUV photoabsorption spectra of pure and mixed CO{\\textless}sub{\\textgreater}2{\\textless}sub/{\\textgreater} and H{\\textless}sub{\\textgreater}2{\\textless}sub/{\\textgreater}O ices exposed to 1 keV electrons at 20 and 80 K to simulate different interstellar and Solar System environments. Ices were then annealed to obtain a layer of pure H{\\textless}sub{\\textgreater}2{\\textless}sub/{\\textgreater}CO{\\textless}sub{\\textgreater}3{\\textless}sub/{\\textgreater} which was further exposed to 1 keV electrons at 20 and 80 K to monitor its destruction pathway. Fourier-transform infrared (FT-IR) spectroscopy was used as a secondary probe providing complementary information on the physicochemical changes within an ice.{\\textless}i{\\textgreater}Results.{\\textless}i/{\\textgreater} Our laboratory work shows that the formation of solid H{\\textless}sub{\\textgreater}2{\\textless}sub/{\\textgreater}CO{\\textless}sub{\\textgreater}3{\\textless}sub/{\\textgreater}, CO, and O{\\textless}sub{\\textgreater}3{\\textless}sub/{\\textgreater} upon the energetic processing of CO{\\textless}sub{\\textgreater}2{\\textless}sub/{\\textgreater}:H{\\textless}sub{\\textgreater}2{\\textless}sub/{\\textgreater}O ice mixtures is temperature-dependent in the range between 20 and 80 K. The amorphous to crystalline phase transition of H{\\textless}sub{\\textgreater}2{\\textless}sub/{\\textgreater}CO{\\textless}sub{\\textgreater}3{\\textless}sub/{\\textgreater} ice is investigated for the first time in the VUV spectral range by annealing the ice at 200 and 225 K. We have detected two photoabsorption bands at 139 and 200 nm, and we assigned them to {\\textless}i{\\textgreater}β{\\textless}i/{\\textgreater}-H{\\textless}sub{\\textgreater}2{\\textless}sub/{\\textgreater}CO{\\textless}sub{\\textgreater}3{\\textless}sub/{\\textgreater} and {\\textless}i{\\textgreater}γ{\\textless}i/{\\textgreater}-H{\\textless}sub{\\textgreater}2{\\textless}sub/{\\textgreater}CO{\\textless}sub{\\textgreater}3{\\textless}sub/{\\textgreater}, respectively. We present VUV spectra of the electron irradiation of annealed H{\\textless}sub{\\textgreater}2{\\textless}sub/{\\textgreater}CO{\\textless}sub{\\textgreater}3{\\textless}sub/{\\textgreater} ice at different temperatures leading to its decomposition into CO{\\textless}sub{\\textgreater}2{\\textless}sub/{\\textgreater}, H{\\textless}sub{\\textgreater}2{\\textless}sub/{\\textgreater}O, and CO ice. Laboratory results are compared to Cassini UltraViolet Imaging Spectrograph observations of the 70−90 K ice surface of Saturn’s satellites Enceladus, Dione, and Rhea.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Astronomy \\& Astrophysics},\n\tauthor = {Ioppolo, S. and Kaňuchová, Z. and James, R. L. and Dawes, A. and Ryabov, A. and Dezalay, J. and Jones, N. C. and Hoffmann, S. V. and Mason, N. J. and Strazzulla, G.},\n\tmonth = feb,\n\tyear = {2021},\n\tpages = {A172},\n}\n\n

\n\n\n

\n \\textlessi\\textgreaterContext.\\textlessi/\\textgreater Carbonic acid (H\\textlesssub\\textgreater2\\textlesssub/\\textgreaterCO\\textlesssub\\textgreater3\\textlesssub/\\textgreater) is a weak acid relevant to astrobiology which, to date, remains undetected in space. Experimental work has shown that the \\textlessi\\textgreaterβ\\textlessi/\\textgreater-polymorph of H\\textlesssub\\textgreater2\\textlesssub/\\textgreaterCO\\textlesssub\\textgreater3\\textlesssub/\\textgreater forms under space relevant conditions through energetic (UV photon, electron, and cosmic ray) processing of CO\\textlesssub\\textgreater2\\textlesssub/\\textgreater- and H\\textlesssub\\textgreater2\\textlesssub/\\textgreaterO-rich ices. Although its \\textlessi\\textgreaterα\\textlessi/\\textgreater-polymorph ice has been recently reassigned to the monomethyl ester of carbonic acid, a different form of H\\textlesssub\\textgreater2\\textlesssub/\\textgreaterCO\\textlesssub\\textgreater3\\textlesssub/\\textgreater ice may exist and is synthesized without irradiation through surface reactions involving CO molecules and OH radicals, that is to say \\textlessi\\textgreaterγ\\textlessi/\\textgreater-H\\textlesssub\\textgreater2\\textlesssub/\\textgreaterCO\\textlesssub\\textgreater3\\textlesssub/\\textgreater.\\textlessi\\textgreaterAims.\\textlessi/\\textgreater We aim to provide a systematic set of vacuum ultraviolet (VUV) photoabsorption spectroscopic data of pure carbonic acid that formed and was destroyed under conditions relevant to space in support of its future identification on the surface of icy objects in the Solar System by the upcoming Jupiter ICy moons Explorer mission and on interstellar dust by the \\textlessi\\textgreaterJames Webb\\textlessi/\\textgreater Space Telescope spacecraft.\\textlessi\\textgreaterMethods.\\textlessi/\\textgreater We present VUV photoabsorption spectra of pure and mixed CO\\textlesssub\\textgreater2\\textlesssub/\\textgreater and H\\textlesssub\\textgreater2\\textlesssub/\\textgreaterO ices exposed to 1 keV electrons at 20 and 80 K to simulate different interstellar and Solar System environments. Ices were then annealed to obtain a layer of pure H\\textlesssub\\textgreater2\\textlesssub/\\textgreaterCO\\textlesssub\\textgreater3\\textlesssub/\\textgreater which was further exposed to 1 keV electrons at 20 and 80 K to monitor its destruction pathway. Fourier-transform infrared (FT-IR) spectroscopy was used as a secondary probe providing complementary information on the physicochemical changes within an ice.\\textlessi\\textgreaterResults.\\textlessi/\\textgreater Our laboratory work shows that the formation of solid H\\textlesssub\\textgreater2\\textlesssub/\\textgreaterCO\\textlesssub\\textgreater3\\textlesssub/\\textgreater, CO, and O\\textlesssub\\textgreater3\\textlesssub/\\textgreater upon the energetic processing of CO\\textlesssub\\textgreater2\\textlesssub/\\textgreater:H\\textlesssub\\textgreater2\\textlesssub/\\textgreaterO ice mixtures is temperature-dependent in the range between 20 and 80 K. The amorphous to crystalline phase transition of H\\textlesssub\\textgreater2\\textlesssub/\\textgreaterCO\\textlesssub\\textgreater3\\textlesssub/\\textgreater ice is investigated for the first time in the VUV spectral range by annealing the ice at 200 and 225 K. We have detected two photoabsorption bands at 139 and 200 nm, and we assigned them to \\textlessi\\textgreaterβ\\textlessi/\\textgreater-H\\textlesssub\\textgreater2\\textlesssub/\\textgreaterCO\\textlesssub\\textgreater3\\textlesssub/\\textgreater and \\textlessi\\textgreaterγ\\textlessi/\\textgreater-H\\textlesssub\\textgreater2\\textlesssub/\\textgreaterCO\\textlesssub\\textgreater3\\textlesssub/\\textgreater, respectively. We present VUV spectra of the electron irradiation of annealed H\\textlesssub\\textgreater2\\textlesssub/\\textgreaterCO\\textlesssub\\textgreater3\\textlesssub/\\textgreater ice at different temperatures leading to its decomposition into CO\\textlesssub\\textgreater2\\textlesssub/\\textgreater, H\\textlesssub\\textgreater2\\textlesssub/\\textgreaterO, and CO ice. Laboratory results are compared to Cassini UltraViolet Imaging Spectrograph observations of the 70−90 K ice surface of Saturn’s satellites Enceladus, Dione, and Rhea.\n

\n\n\n

\n \n\n \n \n \n \n \n \n Emissivity and reflectance spectra at different temperatures of hydrated and anhydrous sulphates: A contribution to investigate the composition and dynamic of icy planetary bodies.\n \n \n \n \n\n\n \n Comodi, P.; Fastelli, M.; Maturilli, A.; Balic-Zunic, T.; and Zucchini, A.\n\n\n \n\n\n\n Icarus, 355: 114132. February 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Emissivity$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{comodi_emissivity_2021,\n\ttitle = {Emissivity and reflectance spectra at different temperatures of hydrated and anhydrous sulphates: {A} contribution to investigate the composition and dynamic of icy planetary bodies},\n\tvolume = {355},\n\tissn = {0019-1035},\n\tshorttitle = {Emissivity and reflectance spectra at different temperatures of hydrated and anhydrous sulphates},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0019103520304747},\n\tdoi = {10.1016/j.icarus.2020.114132},\n\tabstract = {Accurate analyses of existing spacecraft data and telescopic observations are of fundamental importance to describe in detail the surface composition of icy planetary bodies, such as the icy galilean moons. However, the spectral library data to compare the remote data with planetary observations are usually restricted to small spectral ranges and collected only at room temperature. In this study, selected hydrated Mg-sulphates were studied. Emissivity and reflectance spectra were collected in the 3–20 μm and 0.25–16 μm range, respectively, with emissivity collected in the temperature range 300–673 K, and reflectance from 300 to 193 K. All samples were recovered after the heating and cooling cycles and were characterized by means X-ray powder diffraction. Rietveld refinements of the collected data were performed to evaluate the mineralogical composition of the samples before and after the thermal treatment. Both reflectance and emissivity measurements gave us information about the vibrational modes and overtones of SO4 and H2O. Moreover, the careful analysis of the collected data allowed us to study the influence of the cation substitution in the sulphate's crystal structures on the wavelength position of the SO4 vibrational modes. In particular, in simple salts [kieserite MgSO4·(H2O); hexahydrite MgSO4·6(H2O); gypsum CaSO4·2(H2O); thenardite Na2SO4; arcanite K2SO4; anhydrite CaSO4; barite BaSO4], the increase of the cation's radius gives a shift of the ν3 overtone towards higher wavenumbers, varying in the range 1880–2300 cm−1. On the other hand, it was observed that, in hydrated sulphates, that the increase of the strength of the hydrogen bond gives a shift of the ν3(SO4) overtones towards lower wavenumbers. At high temperature, the depth of several absorption bands in the emissivity spectra increases; however, when total or partial de-hydration occurs, a discontinuity in the deepening is observed due to the endothermic character of the dehydration phenomena. Among the investigated samples, several hydrated and anhydrous sulphates undergo de-hydration and/or phase transition at specific temperature conditions. This leads to the stabilization of new crystal structures with higher density compared to the low temperature hydrated ones. The likely occurrence of minerals dehydration will strongly affect the availability of free water in planetary depths and, as a consequence, the thickness of the icy crust. Likewise, the density changes between the different polymorphs will affect the buoyancy. This means that the structural behavior of the “non-icy” components of the icy crust have a significant impact on the structure and dynamics of the planetary bodies and have to be considered in planetological models.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Icarus},\n\tauthor = {Comodi, P. and Fastelli, M. and Maturilli, A. and Balic-Zunic, T. and Zucchini, A.},\n\tmonth = feb,\n\tyear = {2021},\n\tkeywords = {Emissivity measurements, Hydrated salts, Icy bodies, Reflectance measurements, Spectroscopy},\n\tpages = {114132},\n}\n\n

\n\n\n

\n Accurate analyses of existing spacecraft data and telescopic observations are of fundamental importance to describe in detail the surface composition of icy planetary bodies, such as the icy galilean moons. However, the spectral library data to compare the remote data with planetary observations are usually restricted to small spectral ranges and collected only at room temperature. In this study, selected hydrated Mg-sulphates were studied. Emissivity and reflectance spectra were collected in the 3–20 μm and 0.25–16 μm range, respectively, with emissivity collected in the temperature range 300–673 K, and reflectance from 300 to 193 K. All samples were recovered after the heating and cooling cycles and were characterized by means X-ray powder diffraction. Rietveld refinements of the collected data were performed to evaluate the mineralogical composition of the samples before and after the thermal treatment. Both reflectance and emissivity measurements gave us information about the vibrational modes and overtones of SO4 and H2O. Moreover, the careful analysis of the collected data allowed us to study the influence of the cation substitution in the sulphate's crystal structures on the wavelength position of the SO4 vibrational modes. In particular, in simple salts [kieserite MgSO4·(H2O); hexahydrite MgSO4·6(H2O); gypsum CaSO4·2(H2O); thenardite Na2SO4; arcanite K2SO4; anhydrite CaSO4; barite BaSO4], the increase of the cation's radius gives a shift of the ν3 overtone towards higher wavenumbers, varying in the range 1880–2300 cm−1. On the other hand, it was observed that, in hydrated sulphates, that the increase of the strength of the hydrogen bond gives a shift of the ν3(SO4) overtones towards lower wavenumbers. At high temperature, the depth of several absorption bands in the emissivity spectra increases; however, when total or partial de-hydration occurs, a discontinuity in the deepening is observed due to the endothermic character of the dehydration phenomena. Among the investigated samples, several hydrated and anhydrous sulphates undergo de-hydration and/or phase transition at specific temperature conditions. This leads to the stabilization of new crystal structures with higher density compared to the low temperature hydrated ones. The likely occurrence of minerals dehydration will strongly affect the availability of free water in planetary depths and, as a consequence, the thickness of the icy crust. Likewise, the density changes between the different polymorphs will affect the buoyancy. This means that the structural behavior of the “non-icy” components of the icy crust have a significant impact on the structure and dynamics of the planetary bodies and have to be considered in planetological models.\n

\n\n\n

\n \n\n \n \n \n \n \n \n The aqueous alteration of GEMS-like amorphous silicate in a chondritic micrometeorite by Antarctic water.\n \n \n \n \n\n\n \n Suttle, M. D.; Folco, L.; Genge, M. J.; Franchi, I. A.; Campanale, F.; Mugnaioli, E.; and Zhao, X.\n\n\n \n\n\n\n Geochimica et Cosmochimica Acta, 293: 399–421. January 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"The$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{suttle_aqueous_2021,\n\ttitle = {The aqueous alteration of {GEMS}-like amorphous silicate in a chondritic micrometeorite by {Antarctic} water},\n\tvolume = {293},\n\tissn = {0016-7037},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0016703720306815},\n\tdoi = {10.1016/j.gca.2020.11.006},\n\tabstract = {We analysed the heterogenous fine-grained (sub-μm) matrix of a small (58 × 93 μm), unmelted and minimally heated ({\\textless}350 °C) micrometeorite (CP94-050-052) recovered from Antarctic blue ice. This particle contains some unaltered highly primitive phases, including refractory anhydrous high-Mg silicates and submicron crystalline needle-shaped acicular grains interpreted as enstatite whiskers. The particle also contains an abundance of micron-sized Fe-rich grains, which span a compositional and textural continuum between amorphous oxygen-rich silicate and poorly crystalline Fe-rich phyllosilicate (cronstedtite). These Fe-rich grains are here interpreted as secondary phases formed by aqueous alteration. Their inferred anhydrous precursors were likely primitive “GEMS-like” amorphous Fe-Mg-silicates. This micrometeorite’s bulk chemical composition and mineralogy suggest either a carbonaceous chondrite or cometary origin. However, the particle’s average O-isotope composition (δ17O: −12.4‰ [±5.0‰], δ18O: −24.0‰ [±2.3‰] and Δ17O at +0.1‰ [±4.8‰] is distinct from all previously measured chondritic materials. Instead this value is intermediate between primitive chondritic materials and the composition of Antarctic water – strongly implying that the particle was heavily affected by Antarctic alteration. Analysis of the micrometeorite’s H-isotopes reveals low deuterium abundances (δD: −217‰ to −173‰ [±43–47‰]) paired with high H abundances (and thus high water contents [{\\textless}25 wt.\\%]). Although both water contents and H-isotope compositions overlap with those reported in CM chondrites, the datapoints measured from CP94-050-052 extend to more extreme values. Further supporting the idea that the aqueous alteration that affected this micrometeorite operated under different environmental conditions to asteroidal settings. These data collectively demonstrate partial isotopic exchange with light (δ18O-poor, δD-poor) terrestrial fluids whilst the micrometeorite resided in Antarctica. Although this micrometeorite may have been aqueously altered whilst on its parent body this cannot be conclusively demonstrated due to the extent of the weathering overprint. Antarctic alteration operated at significantly higher water-to-rock ratios than chondritic settings. Despite these differences the extent of secondary replacement and the duration of alteration were limited with mafic silicates remaining unaffected. The combined alteration conditions for this particle likely operated over short timescales ({\\textless}24 h), under mildly alkaline conditions (∼pH 8) and at low temperatures ({\\textless}50 °C), this could have occurred during the micrometeorite’s extraction from blue ice.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Geochimica et Cosmochimica Acta},\n\tauthor = {Suttle, M. D. and Folco, L. and Genge, M. J. and Franchi, I. A. and Campanale, F. and Mugnaioli, E. and Zhao, X.},\n\tmonth = jan,\n\tyear = {2021},\n\tkeywords = {Antarctica, Aqueous alteration, GEMS, Micrometeorites, Weathering},\n\tpages = {399--421},\n}\n\n

\n\n\n

\n We analysed the heterogenous fine-grained (sub-μm) matrix of a small (58 × 93 μm), unmelted and minimally heated (\\textless350 °C) micrometeorite (CP94-050-052) recovered from Antarctic blue ice. This particle contains some unaltered highly primitive phases, including refractory anhydrous high-Mg silicates and submicron crystalline needle-shaped acicular grains interpreted as enstatite whiskers. The particle also contains an abundance of micron-sized Fe-rich grains, which span a compositional and textural continuum between amorphous oxygen-rich silicate and poorly crystalline Fe-rich phyllosilicate (cronstedtite). These Fe-rich grains are here interpreted as secondary phases formed by aqueous alteration. Their inferred anhydrous precursors were likely primitive “GEMS-like” amorphous Fe-Mg-silicates. This micrometeorite’s bulk chemical composition and mineralogy suggest either a carbonaceous chondrite or cometary origin. However, the particle’s average O-isotope composition (δ17O: −12.4‰ [±5.0‰], δ18O: −24.0‰ [±2.3‰] and Δ17O at +0.1‰ [±4.8‰] is distinct from all previously measured chondritic materials. Instead this value is intermediate between primitive chondritic materials and the composition of Antarctic water – strongly implying that the particle was heavily affected by Antarctic alteration. Analysis of the micrometeorite’s H-isotopes reveals low deuterium abundances (δD: −217‰ to −173‰ [±43–47‰]) paired with high H abundances (and thus high water contents [\\textless25 wt.%]). Although both water contents and H-isotope compositions overlap with those reported in CM chondrites, the datapoints measured from CP94-050-052 extend to more extreme values. Further supporting the idea that the aqueous alteration that affected this micrometeorite operated under different environmental conditions to asteroidal settings. These data collectively demonstrate partial isotopic exchange with light (δ18O-poor, δD-poor) terrestrial fluids whilst the micrometeorite resided in Antarctica. Although this micrometeorite may have been aqueously altered whilst on its parent body this cannot be conclusively demonstrated due to the extent of the weathering overprint. Antarctic alteration operated at significantly higher water-to-rock ratios than chondritic settings. Despite these differences the extent of secondary replacement and the duration of alteration were limited with mafic silicates remaining unaffected. The combined alteration conditions for this particle likely operated over short timescales (\\textless24 h), under mildly alkaline conditions (∼pH 8) and at low temperatures (\\textless50 °C), this could have occurred during the micrometeorite’s extraction from blue ice.\n

\n\n\n

\n \n\n \n \n \n \n \n \n Sm-Nd isochron ages coupled with C-N isotope data of eclogitic diamonds from Jwaneng, Botswana.\n \n \n \n \n\n\n \n Gress, M. U.; Koornneef, J. M.; Thomassot, E.; Chinn, I. L.; van Zuilen, K.; and Davies, G. R.\n\n\n \n\n\n\n Geochimica et Cosmochimica Acta, 293: 1–17. January 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Sm-Nd$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{gress_sm-nd_2021,\n\ttitle = {Sm-{Nd} isochron ages coupled with {C}-{N} isotope data of eclogitic diamonds from {Jwaneng}, {Botswana}},\n\tvolume = {293},\n\tissn = {0016-7037},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0016703720306426},\n\tdoi = {10.1016/j.gca.2020.10.010},\n\tabstract = {Constraining the formation age of individual diamonds from incorporated mineral inclusions and assessing the host diamonds’ geochemical characteristics allows determination of the complex history of diamond growth in the sub-continental lithospheric mantle (SCLM). It also provides the rare opportunity to study the evolution of the deep cycling of volatiles over time. To achieve these aims, Sm-Nd isotope systematics are presented for 36 eclogitic garnet and clinopyroxene inclusions from 16 diamonds from the Jwaneng mine, Botswana. The inclusions and host diamonds comprise at least two compositional suites that record different ‘mechanisms’ of diamond formation and define two isochrons, one Paleoproterozoic (1.8 Ga) and one Neoproterozoic (0.85 Ga). There are indications of at least three additional diamond-forming events whose ages currently cannot be well constrained. The Paleoproterozoic diamond suite formed by large-scale ({\\textgreater}100′s km), volatile-rich metasomatism related to formation and re-working of the Proto-Kalahari Craton. In contrast, the heterogeneous composition of the Neoproterozoic diamond suite indicates diamond formation on a small-scale, through local ({\\textless}10 km) equilibration of compositionally variable diamond-forming fluids in different eclogitic substrates during the progressive breakup of the Rodinia supercontinent. The results demonstrate that regional events appear to reflect the input of volatiles (i.e., carbon-bearing) derived from the asthenospheric mantle, whereas local diamond-forming events mainly promote the redistribution of volatiles within the SCLM. The occurrence of isotopically light carbon analysed in distinct growth zones from samples of this study (δ13C {\\textless} −21.1‰) provides further indication of a recycled origin for surface-derived carbon in some diamonds from Jwaneng. Determining Earth’s long-term deep carbon cycle using diamonds, however, requires an understanding of the nature and scale of specific diamond-forming events.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Geochimica et Cosmochimica Acta},\n\tauthor = {Gress, M. U. and Koornneef, J. M. and Thomassot, E. and Chinn, I. L. and van Zuilen, K. and Davies, G. R.},\n\tmonth = jan,\n\tyear = {2021},\n\tkeywords = {Carbon and nitrogen isotope, Craton, Diamond, Eclogite, Inclusion dating, Nitrogen aggregation},\n\tpages = {1--17},\n}\n\n

\n\n\n

\n Constraining the formation age of individual diamonds from incorporated mineral inclusions and assessing the host diamonds’ geochemical characteristics allows determination of the complex history of diamond growth in the sub-continental lithospheric mantle (SCLM). It also provides the rare opportunity to study the evolution of the deep cycling of volatiles over time. To achieve these aims, Sm-Nd isotope systematics are presented for 36 eclogitic garnet and clinopyroxene inclusions from 16 diamonds from the Jwaneng mine, Botswana. The inclusions and host diamonds comprise at least two compositional suites that record different ‘mechanisms’ of diamond formation and define two isochrons, one Paleoproterozoic (1.8 Ga) and one Neoproterozoic (0.85 Ga). There are indications of at least three additional diamond-forming events whose ages currently cannot be well constrained. The Paleoproterozoic diamond suite formed by large-scale (\\textgreater100′s km), volatile-rich metasomatism related to formation and re-working of the Proto-Kalahari Craton. In contrast, the heterogeneous composition of the Neoproterozoic diamond suite indicates diamond formation on a small-scale, through local (\\textless10 km) equilibration of compositionally variable diamond-forming fluids in different eclogitic substrates during the progressive breakup of the Rodinia supercontinent. The results demonstrate that regional events appear to reflect the input of volatiles (i.e., carbon-bearing) derived from the asthenospheric mantle, whereas local diamond-forming events mainly promote the redistribution of volatiles within the SCLM. The occurrence of isotopically light carbon analysed in distinct growth zones from samples of this study (δ13C \\textless −21.1‰) provides further indication of a recycled origin for surface-derived carbon in some diamonds from Jwaneng. Determining Earth’s long-term deep carbon cycle using diamonds, however, requires an understanding of the nature and scale of specific diamond-forming events.\n

\n\n\n

\n \n\n \n \n \n \n \n \n Experimental Wind Characterization with the SuperCam Microphone under a Simulated martian Atmosphere.\n \n \n \n \n\n\n \n Chide, B.; Murdoch, N.; Bury, Y.; Maurice, S.; Jacob, X.; Merrison, J. P.; Iversen, J. J.; Meslin, P.; Bassas-Portús, M.; Cadu, A.; Sournac, A.; Dubois, B.; Lorenz, R. D.; Mimoun, D.; and Wiens, R. C.\n\n\n \n\n\n\n Icarus, 354: 114060. January 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Experimental$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{chide_experimental_2021,\n\ttitle = {Experimental {Wind} {Characterization} with the {SuperCam} {Microphone} under a {Simulated} martian {Atmosphere}},\n\tvolume = {354},\n\tissn = {0019-1035},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0019103520304097},\n\tdoi = {10.1016/j.icarus.2020.114060},\n\tabstract = {Located on top of the mast of the Mars 2020 Perseverance rover, the SuperCam instrument suite includes a microphone to record audible sounds from 100Hz to 10kHz on the surface of Mars. It will support SuperCam’s Laser-Induced Breakdown Spectroscopy investigation by recording laser-induced shock-waves but it will also record aeroacoustic noise generated by wind flowing past the microphone. This experimental study was conducted in the Aarhus planetary wind-tunnel under low CO2 pressure with wind generated at several velocities. It focused on understanding the wind-induced acoustic signal measured by microphones instrumented in a real scale model of the rover mast as a function of the wind speed and wind orientation. Acoustic spectra recorded under a wind flow show that the low-frequency range of the microphone signal is mainly influenced by the wind velocity. In contrast, the higher frequency range is seen to depend on the wind direction relative to the microphone. On the one hand, for the wind conditions tested inside the tunnel, it is shown that the Root Mean Square of the pressure, computed over the 100Hz to 500Hz frequency range, is proportional to the dynamic pressure. Therefore, the SuperCam microphone will be able to estimate the wind speed, considering an in situ cross-calibration with the Mars Environmental Dynamic Analyzer. On the other hand, for a given wind speed, it is observed that the root mean square of the pressure, computed over the 500Hz to 2000Hz frequency range, is at its minimum when the microphone is facing the wind whereas it is at its maximum when the microphone is pointing downwind. Hence, a full 360∘ rotation of the mast in azimuth in parallel with sound recording can be used to retrieve the wind direction. We demonstrate that the SuperCam Microphone has a priori the potential to determine both the speed and the direction of the wind on Mars, thus contributing to atmospheric science investigations.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Icarus},\n\tauthor = {Chide, Baptiste and Murdoch, Naomi and Bury, Yannick and Maurice, Sylvestre and Jacob, Xavier and Merrison, Jonathan P. and Iversen, Jens J. and Meslin, Pierre-Yves and Bassas-Portús, Marti and Cadu, Alexandre and Sournac, Anthony and Dubois, Bruno and Lorenz, Ralph D. and Mimoun, David and Wiens, Roger C.},\n\tmonth = jan,\n\tyear = {2021},\n\tkeywords = {Atmosphere, Mars 2020 Perseverance rover, Mars microphone, SuperCam instrument, Wind orientation, Wind speed},\n\tpages = {114060},\n}\n\n

\n\n\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Noble gases in CM carbonaceous chondrites: Effect of parent body aqueous and thermal alteration and cosmic ray exposure ages.\n \n \n \n \n\n\n \n Krietsch, D.; Busemann, H.; Riebe, M. E. I.; King, A. J.; Alexander, C. M. O.; and Maden, C.\n\n\n \n\n\n\n Geochimica et Cosmochimica Acta, 310: 240–280. October 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Noble$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{krietsch_noble_2021,\n\ttitle = {Noble gases in {CM} carbonaceous chondrites: {Effect} of parent body aqueous and thermal alteration and cosmic ray exposure ages},\n\tvolume = {310},\n\tissn = {0016-7037},\n\tshorttitle = {Noble gases in {CM} carbonaceous chondrites},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0016703721003318},\n\tdoi = {10.1016/j.gca.2021.05.050},\n\tabstract = {Like most primitive carbonaceous chondrites, the CM chondrites experienced varying degrees of asteroidal aqueous alteration, which may have overprinted pre-accretionary processing. Several aqueous alteration scales for CM chondrites (and other carbonaceous chondrites) have been proposed based on alteration-dependent changes in various petrological and geochemical characteristics. Given the possibility that the intensity of aqueous alteration could be recorded in the primordial noble gas compositions, we test potential correlations between petrologic, geochemical and noble gas characteristics in a detailed study on 39 CM chondrites, including some of the most pristine CM chondrites identified to date, and 4 CM-related carbonaceous chondrites. We mainly compare our noble gas data with the alteration schemes proposed by Alexander et al. (2013) and Howard et al. (2015). In addition to the noble gas analyses, we determined the phyllosilicate fractions of 17 of the CM chondrites using X-ray diffraction (XRD) to complement missing data points in the Howard alteration scheme. The influence of post-hydration thermal modification on noble gases in CM chondrites is investigated by comparison of heated and unheated samples. Cosmic-ray exposure (CRE) ages are determined for all samples in this study as well as for 26 more samples based on CM chondrite literature noble gas data. The noble gas inventory in CM chondrites represents a mixture of cosmogenic, radiogenic, and abundant primordially trapped noble gases. Additionally, about 50 \\% of our CM bulk samples contain detectable solar wind (SW), which implies that many but not all CM chondrites are regolith breccias or carry SW from a pre-accretion irradiation phase. Aqueous alteration affects primordial noble gas abundances and elemental and isotopic compositions in CM chondrites. In particular, the process causes loss of an Ar-rich component, different in elemental and isotopic composition to known noble gas components. This component is lost during the early stages of aqueous alteration until complete degassing of its carrier material (possibly upon at least partial destruction) below petrologic type of {\\textasciitilde}1.5 on the Howard et al. (2015) scale. Likely, small amounts of Q gases were additionally released by aqueous alteration. Strong thermal modification at {\\textgreater}750 °C results in a significant additional loss of noble gases, whereas peak temperatures {\\textless}500 °C likely have minor effects on the noble gas inventories of CM chondrites. Some of the described trends of noble gas contents and elemental and isotopic ratios in this study are observable across multiple carbonaceous chondrite groups, in particular also the CR chondrites. Hence, these carbonaceous chondrites may have started with similar initial noble gas inventories due to accretion of material from a common reservoir. The CRE ages of most of our CM samples fall within the typical range of {\\textless}10 Myr previously observed for CM chondrites. A few CM chondrites, however, show longer CRE ages, with the longest CRE age of {\\textasciitilde}20Myr determined for the SW-rich CM Allan Hills (ALH) 85013. The degree of aqueous and thermal alteration is variable among CM chondrites with similar CRE ages.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Geochimica et Cosmochimica Acta},\n\tauthor = {Krietsch, Daniela and Busemann, Henner and Riebe, My E. I. and King, Ashley J. and Alexander, Conel M. O'D. and Maden, Colin},\n\tmonth = oct,\n\tyear = {2021},\n\tkeywords = {Aqueous alteration, CM chondrites, Carbonaceous chondrites, Cosmic ray exposure ages, Noble gases, Thermal alteration},\n\tpages = {240--280},\n}\n\n

\n\n\n

\n Like most primitive carbonaceous chondrites, the CM chondrites experienced varying degrees of asteroidal aqueous alteration, which may have overprinted pre-accretionary processing. Several aqueous alteration scales for CM chondrites (and other carbonaceous chondrites) have been proposed based on alteration-dependent changes in various petrological and geochemical characteristics. Given the possibility that the intensity of aqueous alteration could be recorded in the primordial noble gas compositions, we test potential correlations between petrologic, geochemical and noble gas characteristics in a detailed study on 39 CM chondrites, including some of the most pristine CM chondrites identified to date, and 4 CM-related carbonaceous chondrites. We mainly compare our noble gas data with the alteration schemes proposed by Alexander et al. (2013) and Howard et al. (2015). In addition to the noble gas analyses, we determined the phyllosilicate fractions of 17 of the CM chondrites using X-ray diffraction (XRD) to complement missing data points in the Howard alteration scheme. The influence of post-hydration thermal modification on noble gases in CM chondrites is investigated by comparison of heated and unheated samples. Cosmic-ray exposure (CRE) ages are determined for all samples in this study as well as for 26 more samples based on CM chondrite literature noble gas data. The noble gas inventory in CM chondrites represents a mixture of cosmogenic, radiogenic, and abundant primordially trapped noble gases. Additionally, about 50 % of our CM bulk samples contain detectable solar wind (SW), which implies that many but not all CM chondrites are regolith breccias or carry SW from a pre-accretion irradiation phase. Aqueous alteration affects primordial noble gas abundances and elemental and isotopic compositions in CM chondrites. In particular, the process causes loss of an Ar-rich component, different in elemental and isotopic composition to known noble gas components. This component is lost during the early stages of aqueous alteration until complete degassing of its carrier material (possibly upon at least partial destruction) below petrologic type of ~1.5 on the Howard et al. (2015) scale. Likely, small amounts of Q gases were additionally released by aqueous alteration. Strong thermal modification at \\textgreater750 °C results in a significant additional loss of noble gases, whereas peak temperatures \\textless500 °C likely have minor effects on the noble gas inventories of CM chondrites. Some of the described trends of noble gas contents and elemental and isotopic ratios in this study are observable across multiple carbonaceous chondrite groups, in particular also the CR chondrites. Hence, these carbonaceous chondrites may have started with similar initial noble gas inventories due to accretion of material from a common reservoir. The CRE ages of most of our CM samples fall within the typical range of \\textless10 Myr previously observed for CM chondrites. A few CM chondrites, however, show longer CRE ages, with the longest CRE age of ~20Myr determined for the SW-rich CM Allan Hills (ALH) 85013. The degree of aqueous and thermal alteration is variable among CM chondrites with similar CRE ages.\n

\n\n\n

\n \n\n \n \n \n \n \n \n Spectral Properties of H2O Ice Depending on Particle Sizes and Temperatures Expected on Ganymede and Callisto.\n \n \n \n \n\n\n \n Stephan, K.; Ciarniello, M.; Poch, O.; Schmitt, B.; Haack, D.; and Raponi, A.\n\n\n \n\n\n\n ,1341. March 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Spectral$ Paper\n \n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{stephan_spectral_2021,\n\ttitle = {Spectral {Properties} of {H2O} {Ice} {Depending} on {Particle} {Sizes} and {Temperatures} {Expected} on {Ganymede} and {Callisto}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2021LPI....52.1341S},\n\tabstract = {We present the results of laboratory measurements, which were performed in order to evaluate in detail how variations in particle size and surface temperature together influence the spectral H2O-ice signature.},\n\turldate = {2021-07-26},\n\tauthor = {Stephan, K. and Ciarniello, M. and Poch, O. and Schmitt, B. and Haack, D. and Raponi, A.},\n\tmonth = mar,\n\tyear = {2021},\n\tpages = {1341},\n}\n\n

\n\n\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n The Detectability Limit of Organic Molecules within Mars South Polar Laboratory Analogues.\n \n \n \n \n\n\n \n Campbell, J. D.; Schmitt, B.; Brissaud, O.; and Muller, J.\n\n\n \n\n\n\n Journal of Geophysical Research: Planets. June 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"The$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{campbell_detectability_2021,\n\ttitle = {The {Detectability} {Limit} of {Organic} {Molecules} within {Mars} {South} {Polar} {Laboratory} {Analogues}},\n\tissn = {2169-9097, 2169-9100},\n\turl = {https://onlinelibrary.wiley.com/doi/10.1029/2020JE006595},\n\tdoi = {10.1029/2020JE006595},\n\tabstract = {A series of laboratory experiments was carried out in order to generate a diagnostic spectrum for Polycyclic Aromatic Hydrocarbons (PAHs) of astrobiological interest in the context of the Martian South Polar Residual Cap (SPRC), to establish PAH spectral features more easily detectable in CO2 ice (mixed with small amounts of H2O ice) than the previously reported absorption feature at 3.29 µm in order to constrain their detectability limit. There is currently no existing literature on PAH detection within SPRC features, making this work novel and impactful given the recent discovery of a possible subglacial lake beneath the Martian South Pole. Although they have been detected in Martian meteorites, PAHs have not been detected yet on Mars, possibly due to the deleterious effects of ultraviolet radiation on the surface of the planet. SPRC features may provide protection to fragile molecules, and this work seeks to provide laboratory data to improve interpretation of orbital remote sensing spectroscopic imaging data. We also ascertain the effect of CO2 ice sublimation on organic spectra, as well as provide PAH reference spectra in mixtures relevant to Mars. A detectability limit of ∼0.04\\% has been recorded for observing PAHs in CO2 ice using laboratory instrument parameters emulating those of the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM), with new spectral slope features revealed between 0.7 and 1.1 µm, and absorption features at 1.14 and, most sensitively, at 1.685 µm. Mars regolith analogue mixed with a concentration of 1.5\\% PAHs resulted in no discernible organic spectral features. These detectability limits measured in the laboratory are discussed and extrapolated to the effective conditions on the Mars South Polar Cap in terms of dust and water ice abundance and CO2 ice grain size for both the main perennial cap and the H2O ice-dust sublimation lag deposit.},\n\tlanguage = {en},\n\turldate = {2021-06-21},\n\tjournal = {Journal of Geophysical Research: Planets},\n\tauthor = {Campbell, J. D. and Schmitt, B. and Brissaud, O. and Muller, J.‐P.},\n\tmonth = jun,\n\tyear = {2021},\n}\n\n

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\n \n 2020\n \n \n (34)\n \n \n

\n \n \n

\n \n\n \n \n \n \n \n \n Models and data analysis tools for the Solar Orbiter mission.\n \n \n \n \n\n\n \n Rouillard, A. P.; Pinto, R. F.; Vourlidas, A.; De Groof, A.; Thompson, W. T.; Bemporad, A.; Dolei, S.; Indurain, M.; Buchlin, E.; Sasso, C.; Spadaro, D.; Dalmasse, K.; Hirzberger, J.; Zouganelis, I.; Strugarek, A.; Brun, A. S.; Alexandre, M.; Berghmans, D.; Raouafi, N. E.; Wiegelmann, T.; Pagano, P.; Arge, C. N.; Nieves-Chinchilla, T.; Lavarra, M.; Poirier, N.; Amari, T.; Aran, A.; Andretta, V.; Antonucci, E.; Anastasiadis, A.; Auchère, F.; Bellot Rubio, L.; Nicula, B.; Bonnin, X.; Bouchemit, M.; Budnik, E.; Caminade, S.; Cecconi, B.; Carlyle, J.; Cernuda, I.; Davila, J. M.; Etesi, L.; Espinosa Lara, F.; Fedorov, A.; Fineschi, S.; Fludra, A.; Génot, V.; Georgoulis, M. K.; Gilbert, H. R.; Giunta, A.; Gomez-Herrero, R.; Guest, S.; Haberreiter, M.; Hassler, D.; Henney, C. J.; Howard, R. A.; Horbury, T. S.; Janvier, M.; Jones, S. I.; Kozarev, K.; Kraaikamp, E.; Kouloumvakos, A.; Krucker, S.; Lagg, A.; Linker, J.; Lavraud, B.; Louarn, P.; Maksimovic, M.; Maloney, S.; Mann, G.; Masson, A.; Müller, D.; Önel, H.; Osuna, P.; Orozco Suarez, D.; Owen, C. J.; Papaioannou, A.; Pérez-Suárez, D.; Rodriguez-Pacheco, J.; Parenti, S.; Pariat, E.; Peter, H.; Plunkett, S.; Pomoell, J.; Raines, J. M.; Riethmüller, T. L.; Rich, N.; Rodriguez, L.; Romoli, M.; Sanchez, L.; Solanki, S. K.; St Cyr, O. C.; Straus, T.; Susino, R.; Teriaca, L.; Del Toro Iniesta, J. C.; Ventura, R.; Verbeeck, C.; Vilmer, N.; Warmuth, A.; Walsh, A. P.; Watson, C.; Williams, D.; Wu, Y.; and Zhukov, A. N.\n\n\n \n\n\n\n Astronomy & Astrophysics, 642: A2. October 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Models$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{rouillard_models_2020,\n\ttitle = {Models and data analysis tools for the {Solar} {Orbiter} mission},\n\tvolume = {642},\n\tissn = {0004-6361, 1432-0746},\n\turl = {https://www.aanda.org/10.1051/0004-6361/201935305},\n\tdoi = {10.1051/0004-6361/201935305},\n\tabstract = {Context. \n The Solar Orbiter spacecraft will be equipped with a wide range of remote-sensing (RS) and in situ (IS) instruments to record novel and unprecedented measurements of the solar atmosphere and the inner heliosphere. To take full advantage of these new datasets, tools and techniques must be developed to ease multi-instrument and multi-spacecraft studies. In particular the currently inaccessible low solar corona below two solar radii can only be observed remotely. Furthermore techniques must be used to retrieve coronal plasma properties in time and in three dimensional (3D) space. Solar Orbiter will run complex observation campaigns that provide interesting opportunities to maximise the likelihood of linking IS data to their source region near the Sun. Several RS instruments can be directed to specific targets situated on the solar disk just days before data acquisition. To compare IS and RS, data we must improve our understanding of how heliospheric probes magnetically connect to the solar disk. \n \n \n Aims. \n The aim of the present paper is to briefly review how the current modelling of the Sun and its atmosphere can support Solar Orbiter science. We describe the results of a community-led effort by European Space Agency’s Modelling and Data Analysis Working Group (MADAWG) to develop different models, tools, and techniques deemed necessary to test different theories for the physical processes that may occur in the solar plasma. The focus here is on the large scales and little is described with regards to kinetic processes. To exploit future IS and RS data fully, many techniques have been adapted to model the evolving 3D solar magneto-plasma from the solar interior to the solar wind. A particular focus in the paper is placed on techniques that can estimate how Solar Orbiter will connect magnetically through the complex coronal magnetic fields to various photospheric and coronal features in support of spacecraft operations and future scientific studies. \n \n \n Methods. \n Recent missions such as STEREO, provided great opportunities for RS, IS, and multi-spacecraft studies. We summarise the achievements and highlight the challenges faced during these investigations, many of which motivated the Solar Orbiter mission. We present the new tools and techniques developed by the MADAWG to support the science operations and the analysis of the data from the many instruments on Solar Orbiter. \n \n \n Results. \n This article reviews current modelling and tool developments that ease the comparison of model results with RS and IS data made available by current and upcoming missions. It also describes the modelling strategy to support the science operations and subsequent exploitation of Solar Orbiter data in order to maximise the scientific output of the mission. \n \n \n Conclusions. \n The on-going community effort presented in this paper has provided new models and tools necessary to support mission operations as well as the science exploitation of the Solar Orbiter data. The tools and techniques will no doubt evolve significantly as we refine our procedure and methodology during the first year of operations of this highly promising mission.},\n\turldate = {2023-06-29},\n\tjournal = {Astronomy \\& Astrophysics},\n\tauthor = {Rouillard, A. P. and Pinto, R. F. and Vourlidas, A. and De Groof, A. and Thompson, W. T. and Bemporad, A. and Dolei, S. and Indurain, M. and Buchlin, E. and Sasso, C. and Spadaro, D. and Dalmasse, K. and Hirzberger, J. and Zouganelis, I. and Strugarek, A. and Brun, A. S. and Alexandre, M. and Berghmans, D. and Raouafi, N. E. and Wiegelmann, T. and Pagano, P. and Arge, C. N. and Nieves-Chinchilla, T. and Lavarra, M. and Poirier, N. and Amari, T. and Aran, A. and Andretta, V. and Antonucci, E. and Anastasiadis, A. and Auchère, F. and Bellot Rubio, L. and Nicula, B. and Bonnin, X. and Bouchemit, M. and Budnik, E. and Caminade, S. and Cecconi, B. and Carlyle, J. and Cernuda, I. and Davila, J. M. and Etesi, L. and Espinosa Lara, F. and Fedorov, A. and Fineschi, S. and Fludra, A. and Génot, V. and Georgoulis, M. K. and Gilbert, H. R. and Giunta, A. and Gomez-Herrero, R. and Guest, S. and Haberreiter, M. and Hassler, D. and Henney, C. J. and Howard, R. A. and Horbury, T. S. and Janvier, M. and Jones, S. I. and Kozarev, K. and Kraaikamp, E. and Kouloumvakos, A. and Krucker, S. and Lagg, A. and Linker, J. and Lavraud, B. and Louarn, P. and Maksimovic, M. and Maloney, S. and Mann, G. and Masson, A. and Müller, D. and Önel, H. and Osuna, P. and Orozco Suarez, D. and Owen, C. J. and Papaioannou, A. and Pérez-Suárez, D. and Rodriguez-Pacheco, J. and Parenti, S. and Pariat, E. and Peter, H. and Plunkett, S. and Pomoell, J. and Raines, J. M. and Riethmüller, T. L. and Rich, N. and Rodriguez, L. and Romoli, M. and Sanchez, L. and Solanki, S. K. and St Cyr, O. C. and Straus, T. and Susino, R. and Teriaca, L. and Del Toro Iniesta, J. C. and Ventura, R. and Verbeeck, C. and Vilmer, N. and Warmuth, A. and Walsh, A. P. and Watson, C. and Williams, D. and Wu, Y. and Zhukov, A. N.},\n\tmonth = oct,\n\tyear = {2020},\n\tpages = {A2},\n}\n\n

\n\n\n

\n Context. The Solar Orbiter spacecraft will be equipped with a wide range of remote-sensing (RS) and in situ (IS) instruments to record novel and unprecedented measurements of the solar atmosphere and the inner heliosphere. To take full advantage of these new datasets, tools and techniques must be developed to ease multi-instrument and multi-spacecraft studies. In particular the currently inaccessible low solar corona below two solar radii can only be observed remotely. Furthermore techniques must be used to retrieve coronal plasma properties in time and in three dimensional (3D) space. Solar Orbiter will run complex observation campaigns that provide interesting opportunities to maximise the likelihood of linking IS data to their source region near the Sun. Several RS instruments can be directed to specific targets situated on the solar disk just days before data acquisition. To compare IS and RS, data we must improve our understanding of how heliospheric probes magnetically connect to the solar disk. Aims. The aim of the present paper is to briefly review how the current modelling of the Sun and its atmosphere can support Solar Orbiter science. We describe the results of a community-led effort by European Space Agency’s Modelling and Data Analysis Working Group (MADAWG) to develop different models, tools, and techniques deemed necessary to test different theories for the physical processes that may occur in the solar plasma. The focus here is on the large scales and little is described with regards to kinetic processes. To exploit future IS and RS data fully, many techniques have been adapted to model the evolving 3D solar magneto-plasma from the solar interior to the solar wind. A particular focus in the paper is placed on techniques that can estimate how Solar Orbiter will connect magnetically through the complex coronal magnetic fields to various photospheric and coronal features in support of spacecraft operations and future scientific studies. Methods. Recent missions such as STEREO, provided great opportunities for RS, IS, and multi-spacecraft studies. We summarise the achievements and highlight the challenges faced during these investigations, many of which motivated the Solar Orbiter mission. We present the new tools and techniques developed by the MADAWG to support the science operations and the analysis of the data from the many instruments on Solar Orbiter. Results. This article reviews current modelling and tool developments that ease the comparison of model results with RS and IS data made available by current and upcoming missions. It also describes the modelling strategy to support the science operations and subsequent exploitation of Solar Orbiter data in order to maximise the scientific output of the mission. Conclusions. The on-going community effort presented in this paper has provided new models and tools necessary to support mission operations as well as the science exploitation of the Solar Orbiter data. The tools and techniques will no doubt evolve significantly as we refine our procedure and methodology during the first year of operations of this highly promising mission.\n

\n\n\n

\n \n\n \n \n \n \n \n \n Exo-MerCat: A merged exoplanet catalog with Virtual Observatory connection.\n \n \n \n \n\n\n \n Alei, E.; Claudi, R.; Bignamini, A.; and Molinaro, M.\n\n\n \n\n\n\n Astronomy and Computing, 31: 100370. April 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Exo-MerCat:$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{alei_exo-mercat_2020,\n\ttitle = {Exo-{MerCat}: {A} merged exoplanet catalog with {Virtual} {Observatory} connection},\n\tvolume = {31},\n\tissn = {22131337},\n\tshorttitle = {Exo-{MerCat}},\n\turl = {https://linkinghub.elsevier.com/retrieve/pii/S221313371930109X},\n\tdoi = {10.1016/j.ascom.2020.100370},\n\tlanguage = {en},\n\turldate = {2023-06-28},\n\tjournal = {Astronomy and Computing},\n\tauthor = {Alei, E. and Claudi, R. and Bignamini, A. and Molinaro, M.},\n\tmonth = apr,\n\tyear = {2020},\n\tpages = {100370},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Formation of Venus, Earth and Mars: Constrained by Isotopes.\n \n \n \n \n\n\n \n Lammer, H.; Brasser, R.; Johansen, A.; Scherf, M.; and Leitzinger, M.\n\n\n \n\n\n\n Space Science Reviews, 217(1): 7. December 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Formation$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{lammer_formation_2020,\n\ttitle = {Formation of {Venus}, {Earth} and {Mars}: {Constrained} by {Isotopes}},\n\tvolume = {217},\n\tissn = {1572-9672},\n\tshorttitle = {Formation of {Venus}, {Earth} and {Mars}},\n\turl = {https://doi.org/10.1007/s11214-020-00778-4},\n\tdoi = {10.1007/s11214-020-00778-4},\n\tabstract = {Here we discuss the current state of knowledge of terrestrial planet formation from the aspects of different planet formation models and isotopic data from 182Hf-182W, U-Pb, lithophile-siderophile elements, 48Ca/44Ca isotope samples from planetary building blocks, recent reproduction attempts from 36Ar/38Ar, 20Ne/22Ne, 36Ar/22Ne isotope ratios in Venus’ and Earth’s atmospheres, the expected solar 3He abundance in Earth’s deep mantle and Earth’s D/H sea water ratios that shed light on the accretion time of the early protoplanets. Accretion scenarios that can explain the different isotope ratios, including a Moon-forming event ca. 50 Myr after the formation of the Solar System, support the theory that the bulk of Earth’s mass (≥80\\%) most likely accreted within 10–30 Myr. From a combined analysis of the before mentioned isotopes, one finds that proto-Earth accreted most likely a mass of 0.5–0.6 \\$M\\$Earth within the first ≈3–4.5 Myr, the approximate lifetime of the protoplanetary disk. For Venus, the available atmospheric noble gas data are too uncertain for constraining the planet’s accretion scenario accurately. However, from the available imprecise Ar and Ne isotope measurements, one finds that proto-Venus could have grown to a mass of up to 0.85–1.0 \\$M\\$Venus before the disk dissipated. Classical terrestrial planet formation models have struggled to grow large planetary embryos, or even cores of giant planets, quickly from the tiniest materials within the typical lifetime of protoplanetary disks. Pebble accretion could solve this long-standing time scale controversy. Pebble accretion and streaming instabilities produce large planetesimals that grow into Mars-sized and larger planetary embryos during this early accretion phase. The later stage of accretion can be explained well with the Grand-Tack model as well as the annulus and depleted disk models. The relative roles of pebble accretion and planetesimal accretion/giant impacts are poorly understood and should be investigated with N-body simulations that include pebbles and multiple protoplanets. To summarise, different isotopic dating methods and the latest terrestrial planet formation models indicate that the accretion process from dust settling, planetesimal formation, and growth to large planetary embryos and protoplanets is a fast process that occurred to a great extent in the Solar System within the lifetime of the protoplanetary disk.},\n\tlanguage = {en},\n\tnumber = {1},\n\turldate = {2021-09-08},\n\tjournal = {Space Science Reviews},\n\tauthor = {Lammer, Helmut and Brasser, Ramon and Johansen, Anders and Scherf, Manuel and Leitzinger, Martin},\n\tmonth = dec,\n\tyear = {2020},\n\tpages = {7},\n}\n\n

\n\n\n

\n Here we discuss the current state of knowledge of terrestrial planet formation from the aspects of different planet formation models and isotopic data from 182Hf-182W, U-Pb, lithophile-siderophile elements, 48Ca/44Ca isotope samples from planetary building blocks, recent reproduction attempts from 36Ar/38Ar, 20Ne/22Ne, 36Ar/22Ne isotope ratios in Venus’ and Earth’s atmospheres, the expected solar 3He abundance in Earth’s deep mantle and Earth’s D/H sea water ratios that shed light on the accretion time of the early protoplanets. Accretion scenarios that can explain the different isotope ratios, including a Moon-forming event ca. 50 Myr after the formation of the Solar System, support the theory that the bulk of Earth’s mass (≥80%) most likely accreted within 10–30 Myr. From a combined analysis of the before mentioned isotopes, one finds that proto-Earth accreted most likely a mass of 0.5–0.6 $M$Earth within the first ≈3–4.5 Myr, the approximate lifetime of the protoplanetary disk. For Venus, the available atmospheric noble gas data are too uncertain for constraining the planet’s accretion scenario accurately. However, from the available imprecise Ar and Ne isotope measurements, one finds that proto-Venus could have grown to a mass of up to 0.85–1.0 $M$Venus before the disk dissipated. Classical terrestrial planet formation models have struggled to grow large planetary embryos, or even cores of giant planets, quickly from the tiniest materials within the typical lifetime of protoplanetary disks. Pebble accretion could solve this long-standing time scale controversy. Pebble accretion and streaming instabilities produce large planetesimals that grow into Mars-sized and larger planetary embryos during this early accretion phase. The later stage of accretion can be explained well with the Grand-Tack model as well as the annulus and depleted disk models. The relative roles of pebble accretion and planetesimal accretion/giant impacts are poorly understood and should be investigated with N-body simulations that include pebbles and multiple protoplanets. To summarise, different isotopic dating methods and the latest terrestrial planet formation models indicate that the accretion process from dust settling, planetesimal formation, and growth to large planetary embryos and protoplanets is a fast process that occurred to a great extent in the Solar System within the lifetime of the protoplanetary disk.\n

\n\n\n

\n \n\n \n \n \n \n \n \n Did Mars Possess a Dense Atmosphere During the First ${\\}sim400$Million Years?.\n \n \n \n \n\n\n \n Scherf, M.; and Lammer, H.\n\n\n \n\n\n\n Space Science Reviews, 217(1): 2. December 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Did$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{scherf_did_2020,\n\ttitle = {Did {Mars} {Possess} a {Dense} {Atmosphere} {During} the {First} \\${\\textbackslash}sim400\\${Million} {Years}?},\n\tvolume = {217},\n\tissn = {1572-9672},\n\turl = {https://doi.org/10.1007/s11214-020-00779-3},\n\tdoi = {10.1007/s11214-020-00779-3},\n\tabstract = {It is not yet entirely clear whether Mars began as a warm and wet planet that evolved towards the present-day cold and dry body or if it always was cold and dry with just some sporadic episodes of liquid water on its surface. An important clue into this question can be gained by studying the earliest evolution of the Martian atmosphere and whether it was dense and stable to maintain a warm and wet climate or tenuous and susceptible to strong atmospheric escape. In this review we therefore discuss relevant aspects for the evolution and stability of a potential early Martian atmosphere. This contains the EUV flux evolution of the young Sun, the formation timescale and volatile inventory of the planet including volcanic degassing, impact delivery and removal, the loss of the catastrophically outgassed steam atmosphere, atmosphere-surface interactions, as well as thermal and non-thermal escape processes affecting a potential secondary atmosphere at early Mars. While early non-thermal atmospheric escape at Mars before 4 billion years ago is poorly understood, in particular in view of its ancient intrinsic magnetic field, research on thermal escape processes and the stability of a CO2-dominated atmosphere around Mars against high EUV fluxes indicate that volatile delivery and volcanic degassing cannot counterbalance the strong atmospheric escape. Therefore, a catastrophically outgassed steam atmosphere of several bars of CO2 and H2O, or CO and H2 for reduced conditions, through solidification of the Martian magma ocean could have been lost within just a few million years. Thereafter, Mars likely could not build up a dense secondary atmosphere during its first \\${\\textbackslash}sim400\\$million years but might only have possessed an atmosphere sporadically during events of strong volcanic degassing, potentially also including SO2. This indicates that before \\${\\textbackslash}sim4.1\\$billion years ago Mars indeed might have been cold and dry with at maximum short and sporadic warmer periods. A denser CO2- or CO-dominated atmosphere, however, might have built up afterwards but must have been lost later-on due to non-thermal escape processes and sequestration into the ground.},\n\tlanguage = {en},\n\tnumber = {1},\n\turldate = {2021-09-08},\n\tjournal = {Space Science Reviews},\n\tauthor = {Scherf, M. and Lammer, H.},\n\tmonth = dec,\n\tyear = {2020},\n\tpages = {2},\n}\n\n

\n\n\n

\n It is not yet entirely clear whether Mars began as a warm and wet planet that evolved towards the present-day cold and dry body or if it always was cold and dry with just some sporadic episodes of liquid water on its surface. An important clue into this question can be gained by studying the earliest evolution of the Martian atmosphere and whether it was dense and stable to maintain a warm and wet climate or tenuous and susceptible to strong atmospheric escape. In this review we therefore discuss relevant aspects for the evolution and stability of a potential early Martian atmosphere. This contains the EUV flux evolution of the young Sun, the formation timescale and volatile inventory of the planet including volcanic degassing, impact delivery and removal, the loss of the catastrophically outgassed steam atmosphere, atmosphere-surface interactions, as well as thermal and non-thermal escape processes affecting a potential secondary atmosphere at early Mars. While early non-thermal atmospheric escape at Mars before 4 billion years ago is poorly understood, in particular in view of its ancient intrinsic magnetic field, research on thermal escape processes and the stability of a CO2-dominated atmosphere around Mars against high EUV fluxes indicate that volatile delivery and volcanic degassing cannot counterbalance the strong atmospheric escape. Therefore, a catastrophically outgassed steam atmosphere of several bars of CO2 and H2O, or CO and H2 for reduced conditions, through solidification of the Martian magma ocean could have been lost within just a few million years. Thereafter, Mars likely could not build up a dense secondary atmosphere during its first ${\\}sim400$million years but might only have possessed an atmosphere sporadically during events of strong volcanic degassing, potentially also including SO2. This indicates that before ${\\}sim4.1$billion years ago Mars indeed might have been cold and dry with at maximum short and sporadic warmer periods. A denser CO2- or CO-dominated atmosphere, however, might have built up afterwards but must have been lost later-on due to non-thermal escape processes and sequestration into the ground.\n

\n\n\n

\n \n\n \n \n \n \n \n \n A Decade with VAMDC: Results and Ambitions.\n \n \n \n \n\n\n \n Albert, D.; Antony, B. K.; Ba, Y. A.; Babikov, Y. L.; Bollard, P.; Boudon, V.; Delahaye, F.; Del Zanna, G.; Dimitrijević, M. S.; Drouin, B. J.; Dubernet, M.; Duensing, F.; Emoto, M.; Endres, C. P.; Fazliev, A. Z.; Glorian, J.; Gordon, I. E.; Gratier, P.; Hill, C.; Jevremović, D.; Joblin, C.; Kwon, D.; Kochanov, R. V.; Krishnakumar, E.; Leto, G.; Loboda, P. A.; Lukashevskaya, A. A.; Lyulin, O. M.; Marinković, B. P.; Markwick, A.; Marquart, T.; Mason, N. J.; Mendoza, C.; Millar, T. J.; Moreau, N.; Morozov, S. V.; Möller, T.; Müller, H. S. P.; Mulas, G.; Murakami, I.; Pakhomov, Y.; Palmeri, P.; Penguen, J.; Perevalov, V. I.; Piskunov, N.; Postler, J.; Privezentsev, A. I.; Quinet, P.; Ralchenko, Y.; Rhee, Y.; Richard, C.; Rixon, G.; Rothman, L. S.; Roueff, E.; Ryabchikova, T.; Sahal-Bréchot, S.; Scheier, P.; Schilke, P.; Schlemmer, S.; Smith, K. W.; Schmitt, B.; Skobelev, I. Y.; Srecković, V. A.; Stempels, E.; Tashkun, S. A.; Tennyson, J.; Tyuterev, V. G.; Vastel, C.; Vujčić, V.; Wakelam, V.; Walton, N. A.; Zeippen, C.; and Zwölf, C. M.\n\n\n \n\n\n\n Atoms, 8(4): 76. December 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"A$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{albert_decade_2020,\n\ttitle = {A {Decade} with {VAMDC}: {Results} and {Ambitions}},\n\tvolume = {8},\n\tcopyright = {http://creativecommons.org/licenses/by/3.0/},\n\tshorttitle = {A {Decade} with {VAMDC}},\n\turl = {https://www.mdpi.com/2218-2004/8/4/76},\n\tdoi = {10.3390/atoms8040076},\n\tabstract = {This paper presents an overview of the current status of the Virtual Atomic and Molecular Data Centre (VAMDC) e-infrastructure, including the current status of the VAMDC-connected (or to be connected) databases, updates on the latest technological development within the infrastructure and a presentation of some application tools that make use of the VAMDC e-infrastructure. We analyse the past 10 years of VAMDC development and operation, and assess their impact both on the field of atomic and molecular (A\\&amp;M) physics itself and on heterogeneous data management in international cooperation. The highly sophisticated VAMDC infrastructure and the related databases developed over this long term make them a perfect resource of sustainable data for future applications in many fields of research. However, we also discuss the current limitations that prevent VAMDC from becoming the main publishing platform and the main source of A\\&amp;M data for user communities, and present possible solutions under investigation by the consortium. Several user application examples are presented, illustrating the benefits of VAMDC in current research applications, which often need the A\\&amp;M data from more than one database. Finally, we present our vision for the future of VAMDC.},\n\tlanguage = {en},\n\tnumber = {4},\n\turldate = {2021-09-08},\n\tjournal = {Atoms},\n\tauthor = {Albert, Damien and Antony, Bobby K. and Ba, Yaye Awa and Babikov, Yuri L. and Bollard, Philippe and Boudon, Vincent and Delahaye, Franck and Del Zanna, Giulio and Dimitrijević, Milan S. and Drouin, Brian J. and Dubernet, Marie-Lise and Duensing, Felix and Emoto, Masahiko and Endres, Christian P. and Fazliev, Alexandr Z. and Glorian, Jean-Michel and Gordon, Iouli E. and Gratier, Pierre and Hill, Christian and Jevremović, Darko and Joblin, Christine and Kwon, Duck-Hee and Kochanov, Roman V. and Krishnakumar, Erumathadathil and Leto, Giuseppe and Loboda, Petr A. and Lukashevskaya, Anastasiya A. and Lyulin, Oleg M. and Marinković, Bratislav P. and Markwick, Andrew and Marquart, Thomas and Mason, Nigel J. and Mendoza, Claudio and Millar, Tom J. and Moreau, Nicolas and Morozov, Serguei V. and Möller, Thomas and Müller, Holger S. P. and Mulas, Giacomo and Murakami, Izumi and Pakhomov, Yury and Palmeri, Patrick and Penguen, Julien and Perevalov, Valery I. and Piskunov, Nikolai and Postler, Johannes and Privezentsev, Alexei I. and Quinet, Pascal and Ralchenko, Yuri and Rhee, Yong-Joo and Richard, Cyril and Rixon, Guy and Rothman, Laurence S. and Roueff, Evelyne and Ryabchikova, Tatiana and Sahal-Bréchot, Sylvie and Scheier, Paul and Schilke, Peter and Schlemmer, Stephan and Smith, Ken W. and Schmitt, Bernard and Skobelev, Igor Yu and Srecković, Vladimir A. and Stempels, Eric and Tashkun, Serguey A. and Tennyson, Jonathan and Tyuterev, Vladimir G. and Vastel, Charlotte and Vujčić, Veljko and Wakelam, Valentine and Walton, Nicholas A. and Zeippen, Claude and Zwölf, Carlo Maria},\n\tmonth = dec,\n\tyear = {2020},\n\tkeywords = {FAIR principles, atomic and molecular data, interoperability, open access, scientific databases},\n\tpages = {76},\n}\n\n

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\n\n\n

\n \n\n \n \n \n \n \n \n Nitrogen Atmospheres of the Icy Bodies in the Solar System.\n \n \n \n \n\n\n \n Scherf, M.; Lammer, H.; Erkaev, N. V.; Mandt, K. E.; Thaller, S. E.; and Marty, B.\n\n\n \n\n\n\n Space Science Reviews, 216(8): 123. October 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Nitrogen$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{scherf_nitrogen_2020,\n\ttitle = {Nitrogen {Atmospheres} of the {Icy} {Bodies} in the {Solar} {System}},\n\tvolume = {216},\n\tissn = {1572-9672},\n\turl = {https://doi.org/10.1007/s11214-020-00752-0},\n\tdoi = {10.1007/s11214-020-00752-0},\n\tabstract = {This brief review will discuss the current knowledge on the origin and evolution of the nitrogen atmospheres of the icy bodies in the solar system, particularly of Titan, Triton and Pluto. An important tool to analyse and understand the origin and evolution of these atmospheres can be found in the different isotopic signatures of their atmospheric constituents. The 14N/15N ratio of the N2-dominated atmospheres of these bodies serve as a footprint of the building blocks from which Titan, Triton and Pluto originated and of the diverse fractionation processes that shaped these atmospheres over their entire evolution. Together with other measured isotopic and elemental ratios such as 12C/13C or 36Ar/N2 these atmospheres can give important insights into the history of the icy bodies in the solar system, the diverse processes that affect their N2-dominated atmospheres, and the therewith connected solar activity evolution. Titan’s gaseous envelope most likely originated from ammonia ices with possible contributions from refractory organics. Its isotopic signatures can yet be seen in the – compared to Earth – comparatively heavy 14N/15N ratio of 167.7, even though this value slightly evolved over its history due to atmospheric escape and photodissociation of N2. The origin and evolution of Pluto’s and Triton’s tenuous nitrogen atmospheres remain unclear, even though it might be likely that their atmospheres originated from the protosolar nebula or from comets. An in-situ space mission to Triton such as the recently proposed Trident mission, and/or to the ice giants would be a crucial cornerstone for a better understanding of the origin and evolution of the icy bodies in the outer solar system and their atmospheres in general. Due to the importance of the isotopic measurements for understanding the origin and evolution of the icy bodies in the solar system, this review will also give a brief discussion on the diverse isotope measurement techniques with a focus on nitrogen.},\n\tlanguage = {en},\n\tnumber = {8},\n\turldate = {2021-09-08},\n\tjournal = {Space Science Reviews},\n\tauthor = {Scherf, M. and Lammer, H. and Erkaev, N. V. and Mandt, K. E. and Thaller, S. E. and Marty, B.},\n\tmonth = oct,\n\tyear = {2020},\n\tpages = {123},\n}\n\n

\n\n\n

\n This brief review will discuss the current knowledge on the origin and evolution of the nitrogen atmospheres of the icy bodies in the solar system, particularly of Titan, Triton and Pluto. An important tool to analyse and understand the origin and evolution of these atmospheres can be found in the different isotopic signatures of their atmospheric constituents. The 14N/15N ratio of the N2-dominated atmospheres of these bodies serve as a footprint of the building blocks from which Titan, Triton and Pluto originated and of the diverse fractionation processes that shaped these atmospheres over their entire evolution. Together with other measured isotopic and elemental ratios such as 12C/13C or 36Ar/N2 these atmospheres can give important insights into the history of the icy bodies in the solar system, the diverse processes that affect their N2-dominated atmospheres, and the therewith connected solar activity evolution. Titan’s gaseous envelope most likely originated from ammonia ices with possible contributions from refractory organics. Its isotopic signatures can yet be seen in the – compared to Earth – comparatively heavy 14N/15N ratio of 167.7, even though this value slightly evolved over its history due to atmospheric escape and photodissociation of N2. The origin and evolution of Pluto’s and Triton’s tenuous nitrogen atmospheres remain unclear, even though it might be likely that their atmospheres originated from the protosolar nebula or from comets. An in-situ space mission to Triton such as the recently proposed Trident mission, and/or to the ice giants would be a crucial cornerstone for a better understanding of the origin and evolution of the icy bodies in the outer solar system and their atmospheres in general. Due to the importance of the isotopic measurements for understanding the origin and evolution of the icy bodies in the solar system, this review will also give a brief discussion on the diverse isotope measurement techniques with a focus on nitrogen.\n

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\n \n\n \n \n \n \n \n \n Biconical reflectance, micro-Raman, and nano-FTIR spectroscopy of the Didim (H3-5) meteorite: Chemical content and molecular variations.\n \n \n \n \n\n\n \n Yesiltas, M.; Kaya, M.; Glotch, T. D.; Brunetto, R.; Maturilli, A.; Helbert, J.; and Ozel, M. E.\n\n\n \n\n\n\n Meteoritics & Planetary Science, 55(11): 2404–2421. 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Biconical$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{yesiltas_biconical_2020,\n\ttitle = {Biconical reflectance, micro-{Raman}, and nano-{FTIR} spectroscopy of the {Didim} ({H3}-5) meteorite: {Chemical} content and molecular variations},\n\tvolume = {55},\n\tissn = {1945-5100},\n\tshorttitle = {Biconical reflectance, micro-{Raman}, and nano-{FTIR} spectroscopy of the {Didim} ({H3}-5) meteorite},\n\turl = {https://onlinelibrary.wiley.com/doi/abs/10.1111/maps.13585},\n\tdoi = {10.1111/maps.13585},\n\tabstract = {The Didim meteorite contains multiple lithologies and clasts of different petrologic types in a single stone. A mixture of H5 clasts in an unequilibrated H3 host was previously observed in Didim, according to the initial characterization reported in the Meteoritical Bulletin Database, providing an opportunity to investigate molecular composition that contains varying degree of equilibrium with varying mineralogy. We have taken a “from large scale to small scale” approach to spectroscopically investigate the chemical content of Didim. Centimeter-scale biconical reflectance spectra show that Didim contains abundant olivine, pyroxene, and other optically active minerals, evident from a strong Band I near 0.93 µm and a weak Band II near 1.75 µm. Micrometer-scale Raman spectroscopic investigations reveal the presence of carbonaceous material in addition to forsteritic olivine, pyroxene (augite and enstatite), feldspars, and opaque phases such as chromite and hematite. 3-D Raman tomographic imaging shows that the carbonaceous material near chondrules extends underneath a large olivine grain, going further down toward the interior, indicating that the observed carbonaceous matter is likely indigenous. Nano-scale infrared measurements reveal that the observed chemical materials in Didim contain spectral, and therefore, molecular, variations at the 20 nm spatial scale. These chemical variations are normally not accessible via conventional infrared techniques, and indicate the presence of different cations in the molecular composition of observed minerals. By taking the “large scale to small scale” approach, we show that these compositional variations can be captured and investigated nondestructively in meteorites to understand formation/evolution of chemical components in the parent body.},\n\tlanguage = {en},\n\tnumber = {11},\n\turldate = {2021-09-08},\n\tjournal = {Meteoritics \\& Planetary Science},\n\tauthor = {Yesiltas, M. and Kaya, M. and Glotch, T. D. and Brunetto, R. and Maturilli, A. and Helbert, J. and Ozel, M. E.},\n\tyear = {2020},\n\tpages = {2404--2421},\n}\n\n

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\n \n\n \n \n \n \n \n \n Effect of impact shock on extremophilic Halomonas gomseoemensis EP-3 isolated from hypersaline sulphated lake Laguna de Peña Hueca, Spain.\n \n \n \n \n\n\n \n Thombre, R S; Gomez, F.; Parkhe, R.; Kaur, K.; Vaishampayan, P.; Shivakarthik, E.; Sivaraman, B.; Perumal, R.; and Mason, N.\n\n\n \n\n\n\n Planetary and Space Science, 192: 105041. November 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Effect$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{thombre_effect_2020,\n\ttitle = {Effect of impact shock on extremophilic {Halomonas} gomseoemensis {EP}-3 isolated from hypersaline sulphated lake {Laguna} de {Peña} {Hueca}, {Spain}},\n\tvolume = {192},\n\tissn = {0032-0633},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0032063319305513},\n\tdoi = {10.1016/j.pss.2020.105041},\n\tabstract = {The geologic histories of planetary surfaces reveal that Earth and Mars have been pummeled by cataclysmic impact events. The surface of Mars has been perused to have an impact origin for its hemispheric dichotomy. The spallation during impact events causes the interplanetary transfer of material from Mars to Earth or Mars to Phobos/Deimos. Assessing the survival of micro-organisms in impact conditions is critical for the development of planetary protection strategies for future missions. Shock waves are generated during such major impact events. The objective of the present investigation was to explore the microbial diversity of the hypersaline sulphated Laguna de Peña Hueca, Spain and to study the effect of shock waves on extremophilic bacteria isolated from the lake. Peña Hueca is a hypersaline sulphated lagoon rich in Mg–Na–SO4–Cl, epsomite and hexahydrate and it potentially serves as Planetary field analogue site for Martian chloride deposits and salt-rich subsurface brines of Ocean worlds like Enceladus and Europa. The microbial community structure of the lagoon was studied by 16S rRNA metagenomic sequencing. The phylogenetic studies indicated the presence of phyla Euryarchaeota, Proteobacteria, and Bacteroides in the hypersaline brines of the lagoon. The anoxic sediments of Peña Hueca showed the presence of Haloanaerobiaeta and Hadesarchaeota including the anoxic genus of Haloanaerobium, Desulfosalsimonas and Desulfovermiculum. The effect of impact shock on the halophilic bacterium Halomonas gomseomensis EP-3 isolated from Laguna de Peña Hueca was studied in a Reddy shock tube. The halophilic bacterium was exposed to shock waves at a peak shock pressure of 300 kPa and a temperature of 400 K. The results of shock recovery experiments of halophilic bacteria reveal 97\\% killing at 300 kPa and Mach number of 1.47 in comparison with Bacillus sp. This study indicates that gram-positive spore-forming Bacillus sp. are better adapted to survival in impact shock waves in comparison to non-sporulating halophiles. In the current study, we present the first report on response of halophiles in impact shock. Furthermore, we demonstrate a novel application of the simple handheld Reddy shock tube in astrobiology. The survival studies of halophiles isolated from terrestrial analogue sites in impact shock can provide valuable insights in astrobiology and microbial physiology in impact shock stress.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Planetary and Space Science},\n\tauthor = {Thombre, R S and Gomez, F. and Parkhe, R. and Kaur, K. and Vaishampayan, P. and Shivakarthik, E. and Sivaraman, B. and Perumal, R. and Mason, N.},\n\tmonth = nov,\n\tyear = {2020},\n\tkeywords = {Astrobiology, Habitability, Hypersaline, Impact, Mars analogue, Microbial community, Ocean world, Reddy shock tube, Shock waves},\n\tpages = {105041},\n}\n\n

\n\n\n

\n The geologic histories of planetary surfaces reveal that Earth and Mars have been pummeled by cataclysmic impact events. The surface of Mars has been perused to have an impact origin for its hemispheric dichotomy. The spallation during impact events causes the interplanetary transfer of material from Mars to Earth or Mars to Phobos/Deimos. Assessing the survival of micro-organisms in impact conditions is critical for the development of planetary protection strategies for future missions. Shock waves are generated during such major impact events. The objective of the present investigation was to explore the microbial diversity of the hypersaline sulphated Laguna de Peña Hueca, Spain and to study the effect of shock waves on extremophilic bacteria isolated from the lake. Peña Hueca is a hypersaline sulphated lagoon rich in Mg–Na–SO4–Cl, epsomite and hexahydrate and it potentially serves as Planetary field analogue site for Martian chloride deposits and salt-rich subsurface brines of Ocean worlds like Enceladus and Europa. The microbial community structure of the lagoon was studied by 16S rRNA metagenomic sequencing. The phylogenetic studies indicated the presence of phyla Euryarchaeota, Proteobacteria, and Bacteroides in the hypersaline brines of the lagoon. The anoxic sediments of Peña Hueca showed the presence of Haloanaerobiaeta and Hadesarchaeota including the anoxic genus of Haloanaerobium, Desulfosalsimonas and Desulfovermiculum. The effect of impact shock on the halophilic bacterium Halomonas gomseomensis EP-3 isolated from Laguna de Peña Hueca was studied in a Reddy shock tube. The halophilic bacterium was exposed to shock waves at a peak shock pressure of 300 kPa and a temperature of 400 K. The results of shock recovery experiments of halophilic bacteria reveal 97% killing at 300 kPa and Mach number of 1.47 in comparison with Bacillus sp. This study indicates that gram-positive spore-forming Bacillus sp. are better adapted to survival in impact shock waves in comparison to non-sporulating halophiles. In the current study, we present the first report on response of halophiles in impact shock. Furthermore, we demonstrate a novel application of the simple handheld Reddy shock tube in astrobiology. The survival studies of halophiles isolated from terrestrial analogue sites in impact shock can provide valuable insights in astrobiology and microbial physiology in impact shock stress.\n

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\n \n\n \n \n \n \n \n \n Filtration of simulated Martian atmosphere for in-situ oxygen production.\n \n \n \n \n\n\n \n McClean, J. B.; Merrison, J. P.; Iversen, J. J.; Azimian, M.; Wiegmann, A.; Pike, W. T.; and Hecht, M. H.\n\n\n \n\n\n\n Planetary and Space Science, 191: 104975. October 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Filtration$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{mcclean_filtration_2020,\n\ttitle = {Filtration of simulated {Martian} atmosphere for in-situ oxygen production},\n\tvolume = {191},\n\tissn = {0032-0633},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0032063319300698},\n\tdoi = {10.1016/j.pss.2020.104975},\n\tabstract = {In-Situ Resource Utilisation (ISRU) can reduce the mass and cost of planetary missions. The Mars Oxygen ISRU Experiment (MOXIE) on the Mars 2020 rover Perseverance will demonstrate ISRU on Mars for the first time by producing oxygen from atmospheric carbon dioxide via solid oxide electrolysis. To protect the solid oxide electrolysis subsystem from contamination by dust, a High Efficiency Particulate Air (HEPA) filter is used. However, the performance of HEPA filters in Martian atmospheric conditions is not well understood. The theory of filtration was reviewed in the context of filtration of Mars’ atmosphere, and an experimental investigation was carried out to determine the dust loading rate and pressure drop as a function of dust loading and filtration velocity for a flight-representative pleated and baffled MOXIE HEPA filter using wind tunnels and Martian dust simulant. In simulated atmospheric conditions of 10.3 mbar carbon dioxide at room temperature with a horizontal wind speed of 3 m s−1 and filter inlet face velocity of 7.1 cm s−1, the dust loading rate was (0.19 ± 0.02) mg m−2 h−1. This is likely a lower bound: analytical approaches estimate dust loading rates of up to approximately 20 mg m−2 h−1. The pressure drop ΔP (mbar) as a function of dust loading m (g m−2) and filtration velocity UF (cm s−1) was ΔP=am+bUF, where a = 0.0012(1)mbar (g m-2)-1 (cm s-1)-1 and b = 0.063(1) mbar (cm s-1)-1. Due to operation outside the continuum flow regime, pressure drop increased with atmospheric pressure, unlike HEPA filters on Earth where pressure drop is independent of atmospheric pressure. Dust is unlikely to produce a problematic pressure drop for MOXIE, but needs to be considered for large-scale filtration if the benefits of atmospheric ISRU on Mars are to be fully realised.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Planetary and Space Science},\n\tauthor = {McClean, J. B. and Merrison, J. P. and Iversen, J. J. and Azimian, M. and Wiegmann, A. and Pike, W. T. and Hecht, M. H.},\n\tmonth = oct,\n\tyear = {2020},\n\tkeywords = {Dust, Filtration, In-situ resource utilisation, Mars},\n\tpages = {104975},\n}\n\n

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\n \n\n \n \n \n \n \n \n Analyzing the Performance of a Miniature 3D Wind Sensor for Mars.\n \n \n \n \n\n\n \n Domínguez-Pumar, M.; Kowalski, L.; Jiménez, V.; Rodríguez, I.; Soria, M.; Bermejo, S.; and Pons-Nin, J.\n\n\n \n\n\n\n Sensors, 20(20): 5912. January 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Analyzing$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{dominguez-pumar_analyzing_2020,\n\ttitle = {Analyzing the {Performance} of a {Miniature} {3D} {Wind} {Sensor} for {Mars}},\n\tvolume = {20},\n\tcopyright = {http://creativecommons.org/licenses/by/3.0/},\n\turl = {https://www.mdpi.com/1424-8220/20/20/5912},\n\tdoi = {10.3390/s20205912},\n\tabstract = {This paper analyzes the behavior of a miniature 3D wind sensor designed for Mars atmosphere. The sensor is a spherical structure of 10 mm diameter divided in four sectors. By setting all the sectors to constant temperature, above that of the air, the 3D wind velocity vector can be measured. Two sets of experiments have been performed. First, an experimental campaign made under typical Mars conditions at the Aarhus Wind Tunnel Simulator is presented. The results demonstrate that both wind speed and angle can be efficiently measured, using a simple inverse algorithm. The effect of sudden wind changes is also analyzed and fast response times in the range of 0.7 s are obtained. The second set of experiments is focused on analyzing the performance of the sensor under extreme Martian wind conditions, reaching and going beyond the Dust Devil scale. To this purpose, both high-fidelity numerical simulations of fluid dynamics and heat transfer and experiments with the sensor have been performed. The results of the experiments, made for winds in the Reynolds number 1000\\&ndash;2000 range, which represent 65\\&ndash;130 m/s of wind speed under typical Mars conditions, further confirm the simulation predictions and show that it will be possible to successfully measure wind speed and direction even under these extreme regimes.},\n\tlanguage = {en},\n\tnumber = {20},\n\turldate = {2021-09-08},\n\tjournal = {Sensors},\n\tauthor = {Domínguez-Pumar, Manuel and Kowalski, Lukasz and Jiménez, Vicente and Rodríguez, Ivette and Soria, Manel and Bermejo, Sandra and Pons-Nin, Joan},\n\tmonth = jan,\n\tyear = {2020},\n\tkeywords = {heat transfer, low pressure atmosphere, mars exploration, spherical sensors, thermal anemometry, wind sensors},\n\tpages = {5912},\n}\n\n

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\n \n\n \n \n \n \n \n \n The tungsten-182 record of kimberlites above the African superplume: Exploring links to the core-mantle boundary.\n \n \n \n \n\n\n \n Tappe, S.; Budde, G.; Stracke, A.; Wilson, A.; and Kleine, T.\n\n\n \n\n\n\n Earth and Planetary Science Letters, 547: 116473. October 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"The$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{tappe_tungsten-182_2020,\n\ttitle = {The tungsten-182 record of kimberlites above the {African} superplume: {Exploring} links to the core-mantle boundary},\n\tvolume = {547},\n\tissn = {0012-821X},\n\tshorttitle = {The tungsten-182 record of kimberlites above the {African} superplume},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0012821X20304179},\n\tdoi = {10.1016/j.epsl.2020.116473},\n\tabstract = {Many volcanic hotspots are connected via ‘plume’ conduits to thermochemical structures with anomalously low seismic velocities at the core-mantle boundary. Basaltic lavas from some of these hotspots show anomalous daughter isotope abundances for the short-lived 129I-129Xe, 146Sm-142Nd, and 182Hf-182W radioactive decay systems, suggesting that their lower mantle sources contain material that dates back to Earth-forming events during the first 100 million years in solar system history. Survival of such ‘primordial’ remnants in Earth's mantle places important constraints on the evolution and inner workings of terrestrial planets. Here we report high-precision 182W/184W measurements for a large suite of kimberlite volcanic rocks from across the African tectonic plate, which for the past 250 million years has drifted over the most prominent thermochemical seismic anomaly at the core-mantle boundary. This so-called African LLSVP, or ‘large low shear-wave velocity province’, is widely suspected to store early Earth remnants and is implicated as the ultimate source of global Phanerozoic kimberlite magmatism. Our results show, however, that kimberlites from above the African LLSVP, including localities with lower mantle diamonds such as Letseng and Karowe Orapa A/K6, lack anomalous 182W signatures, with an average μ182W value of 0.0 ± 4.1 (2SD) for the 18 occurrences studied. If kimberlites are indeed sourced from the African LLSVP or superplume, then the extensive 182W evidence suggests that primordial or core-equilibrated mantle materials, which may contribute resolvable μ182W excesses or deficits, are only minor or locally concentrated components in the lowermost mantle, for example in the much smaller ‘ultra-low velocity zones’ or ULVZs. However, the lack of anomalous 182W may simply suggest that low-volume kimberlite magmas are not derived from hot lower mantle plumes. In this alternative scenario, kimberlite magmas originate from volatile-fluxed ambient convecting upper mantle domains beneath relatively thick and cold lithosphere from where previously ‘stranded’ lower mantle and transition zone diamonds can be plucked.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Earth and Planetary Science Letters},\n\tauthor = {Tappe, Sebastian and Budde, Gerrit and Stracke, Andreas and Wilson, Allan and Kleine, Thorsten},\n\tmonth = oct,\n\tyear = {2020},\n\tkeywords = {LLSVP, extinct radionuclides, kimberlite origin, plate tectonics, primordial mantle reservoirs, ultradeep diamonds},\n\tpages = {116473},\n}\n\n

\n\n\n

\n Many volcanic hotspots are connected via ‘plume’ conduits to thermochemical structures with anomalously low seismic velocities at the core-mantle boundary. Basaltic lavas from some of these hotspots show anomalous daughter isotope abundances for the short-lived 129I-129Xe, 146Sm-142Nd, and 182Hf-182W radioactive decay systems, suggesting that their lower mantle sources contain material that dates back to Earth-forming events during the first 100 million years in solar system history. Survival of such ‘primordial’ remnants in Earth's mantle places important constraints on the evolution and inner workings of terrestrial planets. Here we report high-precision 182W/184W measurements for a large suite of kimberlite volcanic rocks from across the African tectonic plate, which for the past 250 million years has drifted over the most prominent thermochemical seismic anomaly at the core-mantle boundary. This so-called African LLSVP, or ‘large low shear-wave velocity province’, is widely suspected to store early Earth remnants and is implicated as the ultimate source of global Phanerozoic kimberlite magmatism. Our results show, however, that kimberlites from above the African LLSVP, including localities with lower mantle diamonds such as Letseng and Karowe Orapa A/K6, lack anomalous 182W signatures, with an average μ182W value of 0.0 ± 4.1 (2SD) for the 18 occurrences studied. If kimberlites are indeed sourced from the African LLSVP or superplume, then the extensive 182W evidence suggests that primordial or core-equilibrated mantle materials, which may contribute resolvable μ182W excesses or deficits, are only minor or locally concentrated components in the lowermost mantle, for example in the much smaller ‘ultra-low velocity zones’ or ULVZs. However, the lack of anomalous 182W may simply suggest that low-volume kimberlite magmas are not derived from hot lower mantle plumes. In this alternative scenario, kimberlite magmas originate from volatile-fluxed ambient convecting upper mantle domains beneath relatively thick and cold lithosphere from where previously ‘stranded’ lower mantle and transition zone diamonds can be plucked.\n

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\n \n\n \n \n \n \n \n \n Isotopic and textural analysis of giant unmelted micrometeorites – identification of new material from intensely altered 16O-poor water-rich asteroids.\n \n \n \n \n\n\n \n Suttle, M. D.; Dionnet, Z.; Franchi, I.; Folco, L.; Gibson, J.; Greenwood, R. C.; Rotundi, A.; King, A.; and Russell, S. S.\n\n\n \n\n\n\n Earth and Planetary Science Letters, 546: 116444. September 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Isotopic$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{suttle_isotopic_2020,\n\ttitle = {Isotopic and textural analysis of giant unmelted micrometeorites – identification of new material from intensely altered {16O}-poor water-rich asteroids},\n\tvolume = {546},\n\tissn = {0012-821X},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0012821X20303885},\n\tdoi = {10.1016/j.epsl.2020.116444},\n\tabstract = {Bulk oxygen isotope data has the potential to match extraterrestrial samples to parent body sources based on distinctive δ18O and Δ17O ratios. We analysed 10 giant ({\\textgreater}500 μm) micrometeorites using combined micro-Computer Tomography (μCT) and O-isotope analysis to pair internal textures to inferred parent body groups. We identify three ordinary chondrite particles (L and LL groups), four from CR chondrites and the first micrometeorite from the enstatite chondrite (EH4) group. In addition, two micrometeorites are from hydrated carbonaceous chondrite parent bodies with 16O-poor isotopic compositions and plot above the terrestrial fractionation line. They experienced intense aqueous alteration, contain pseudomorphic chondrules and are petrographically similar to the CM1/CR1 chondrites. These micrometeorites may be members of the newly established CY chondrites and/or derived from the enigmatic “Group 4” micrometeorite population, previously identified by Yada et al., 2005 [GCA, 69:5789-5804], Suavet et al., 2010 [EPSL, 293:313-320] (and others). One of our 16O-poor micrometeorite plots on the same isotopic trendline as the CO, CM and CY chondrites – “the CM mixing line” (with a slope of ∼0.7 and a δ17O intercept of -4.23‰), this implies a close relationship and potentially a genetic link to these hydrated chondrites. If position along the CM mixing line reflects the amount of 16O-poor (heavy) water-ice accreted onto the parent body at formation, then the CY chondrites and these 16O-poor micrometeorites must have accreted at least as much water-ice as CM chondrites but potentially more. In addition, thermal metamorphism could have played a role in further raising the bulk O-isotope compositions through the preferential loss of isotopically light water during phyllosilicate dehydration. The study of micrometeorites provides insights into asteroid belt diversity through the discovery of material not currently sampled by larger meteorites, perhaps as a result of atmospheric entry biases preventing the survival of large blocks of friable hydrated material.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Earth and Planetary Science Letters},\n\tauthor = {Suttle, M. D. and Dionnet, Z. and Franchi, I. and Folco, L. and Gibson, J. and Greenwood, R. C. and Rotundi, A. and King, A. and Russell, S. S.},\n\tmonth = sep,\n\tyear = {2020},\n\tkeywords = {O-isotopes, carbonaceous chondrites, micrometeorites, water-to-rock ratio},\n\tpages = {116444},\n}\n\n

\n\n\n

\n Bulk oxygen isotope data has the potential to match extraterrestrial samples to parent body sources based on distinctive δ18O and Δ17O ratios. We analysed 10 giant (\\textgreater500 μm) micrometeorites using combined micro-Computer Tomography (μCT) and O-isotope analysis to pair internal textures to inferred parent body groups. We identify three ordinary chondrite particles (L and LL groups), four from CR chondrites and the first micrometeorite from the enstatite chondrite (EH4) group. In addition, two micrometeorites are from hydrated carbonaceous chondrite parent bodies with 16O-poor isotopic compositions and plot above the terrestrial fractionation line. They experienced intense aqueous alteration, contain pseudomorphic chondrules and are petrographically similar to the CM1/CR1 chondrites. These micrometeorites may be members of the newly established CY chondrites and/or derived from the enigmatic “Group 4” micrometeorite population, previously identified by Yada et al., 2005 [GCA, 69:5789-5804], Suavet et al., 2010 [EPSL, 293:313-320] (and others). One of our 16O-poor micrometeorite plots on the same isotopic trendline as the CO, CM and CY chondrites – “the CM mixing line” (with a slope of ∼0.7 and a δ17O intercept of -4.23‰), this implies a close relationship and potentially a genetic link to these hydrated chondrites. If position along the CM mixing line reflects the amount of 16O-poor (heavy) water-ice accreted onto the parent body at formation, then the CY chondrites and these 16O-poor micrometeorites must have accreted at least as much water-ice as CM chondrites but potentially more. In addition, thermal metamorphism could have played a role in further raising the bulk O-isotope compositions through the preferential loss of isotopically light water during phyllosilicate dehydration. The study of micrometeorites provides insights into asteroid belt diversity through the discovery of material not currently sampled by larger meteorites, perhaps as a result of atmospheric entry biases preventing the survival of large blocks of friable hydrated material.\n

\n\n\n

\n \n\n \n \n \n \n \n \n Style and intensity of hydration among C-complex asteroids: A comparison to desiccated carbonaceous chondrites.\n \n \n \n \n\n\n \n Potin, S.; Beck, P.; Usui, F.; Bonal, L.; Vernazza, P.; and Schmitt, B.\n\n\n \n\n\n\n Icarus, 348: 113826. September 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Style$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{potin_style_2020,\n\ttitle = {Style and intensity of hydration among {C}-complex asteroids: {A} comparison to desiccated carbonaceous chondrites},\n\tvolume = {348},\n\tissn = {0019-1035},\n\tshorttitle = {Style and intensity of hydration among {C}-complex asteroids},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0019103520302086},\n\tdoi = {10.1016/j.icarus.2020.113826},\n\tabstract = {Here we report a comparison between reflectance spectroscopy of meteorites under asteroidal environment (high vacuum and temperature) and Main Belt and Near Earth Asteroids spectra. Focusing on the –OH absorption feature around 3 μm, we show that the asteroidal environment induces a reduction of depth and width of the band, as well as a shift of the reflectance minimum. We then decompose the –OH feature into several components with a new model using Exponentially Modified Gaussians. Unlike previous studies, we confirme the link between these components, the aqueous alteration history and the amount of water molecules inside of the sample, using the shape of this spectral feature only. We then apply this deconvolution model to asteroids spectra which were obtained with a space-borne telescope and two space probes, and find a strong similarity with the components detected on meteorites, and among asteroids from a same type. Based on the conclusions drawn from our meteorites experiment, we suggest to use the 3-μm band as a tracer of the alteration history of the small bodies. Using the 3-μm band only, we show that Ryugu has been heavily altered by water, which is consistent with its parent body being covered with water ice, then went through a high temperature sequence, over 400 °C. We also point out that the 3-μm band of Bennu shows signs of its newly discovered surface activity.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Icarus},\n\tauthor = {Potin, S. and Beck, P. and Usui, F. and Bonal, L. and Vernazza, P. and Schmitt, B.},\n\tmonth = sep,\n\tyear = {2020},\n\tkeywords = {Asteroids, Meteorites, Spectroscopy, Surfaces, Thermal alteration},\n\tpages = {113826},\n}\n\n

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\n \n\n \n \n \n \n \n \n Vacuum ultraviolet photoabsorption spectroscopy of space-related ices: 1 keV electron irradiation of nitrogen- and oxygen-rich ices.\n \n \n \n \n\n\n \n Ioppolo, S.; Kaňuchová, Z.; James, R. L.; Dawes, A.; Jones, N. C.; Hoffmann, S. V.; Mason, N. J.; and Strazzulla, G.\n\n\n \n\n\n\n Astronomy & Astrophysics, 641: A154. September 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Vacuum$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{ioppolo_vacuum_2020,\n\ttitle = {Vacuum ultraviolet photoabsorption spectroscopy of space-related ices: 1 {keV} electron irradiation of nitrogen- and oxygen-rich ices},\n\tvolume = {641},\n\tcopyright = {© ESO 2020},\n\tissn = {0004-6361, 1432-0746},\n\tshorttitle = {Vacuum ultraviolet photoabsorption spectroscopy of space-related ices},\n\turl = {https://www.aanda.org/articles/aa/abs/2020/09/aa35477-19/aa35477-19.html},\n\tdoi = {10.1051/0004-6361/201935477},\n\tabstract = {{\\textless}i{\\textgreater}Context.{\\textless}i/{\\textgreater} Molecular oxygen, nitrogen, and ozone have been detected on some satellites of Saturn and Jupiter, as well as on comets. They are also expected to be present in ice-grain mantles within star-forming regions. The continuous energetic processing of icy objects in the Solar System induces physical and chemical changes within the ice. Laboratory experiments that simulate energetic processing (ions, photons, and electrons) of ices are therefore essential for interpreting and directing future astronomical observations.{\\textless}i{\\textgreater}Aims.{\\textless}i/{\\textgreater} We provide vacuum ultraviolet (VUV) photoabsorption spectroscopic data of energetically processed nitrogen- and oxygen-rich ices that will help to identify absorption bands and/or spectral slopes observed on icy objects in the Solar System and on ice-grain mantles of the interstellar medium.{\\textless}i{\\textgreater}Methods.{\\textless}i/{\\textgreater} We present VUV photoabsorption spectra of frozen O{\\textless}sub{\\textgreater}2{\\textless}sub/{\\textgreater} and N{\\textless}sub{\\textgreater}2{\\textless}sub/{\\textgreater}, a 1:1 mixture of both, and a new systematic set of pure and mixed nitrogen oxide ices. Spectra were obtained at 22 K before and after 1 keV electron bombardment of the ice sample. Ices were then annealed to higher temperatures to study their thermal evolution. In addition, Fourier-transform infrared spectroscopy was used as a secondary probe of molecular synthesis to better identify the physical and chemical processes at play.{\\textless}i{\\textgreater}Results.{\\textless}i/{\\textgreater} Our VUV data show that ozone and the azide radical (N{\\textless}sub{\\textgreater}3{\\textless}sub/{\\textgreater}) are observed in our experiments after electron irradiation of pure O{\\textless}sub{\\textgreater}2{\\textless}sub/{\\textgreater} and N{\\textless}sub{\\textgreater}2{\\textless}sub/{\\textgreater} ices, respectively. Energetic processing of an O{\\textless}sub{\\textgreater}2{\\textless}sub/{\\textgreater}:N{\\textless}sub{\\textgreater}2{\\textless}sub/{\\textgreater} = 1:1 ice mixture leads to the formation of ozone along with a series of nitrogen oxides. The electron irradiation of solid nitrogen oxides, pure and in mixtures, induces the formation of new species such as O{\\textless}sub{\\textgreater}2{\\textless}sub/{\\textgreater}, N{\\textless}sub{\\textgreater}2{\\textless}sub/{\\textgreater}, and other nitrogen oxides not present in the initial ice. Results are discussed here in light of their relevance to various astrophysical environments. Finally, we show that VUV spectra of solid NO{\\textless}sub{\\textgreater}2{\\textless}sub/{\\textgreater} and water can reproduce the observational VUV profile of the cold surface of Enceladus, Dione, and Rhea, strongly suggesting the presence of nitrogen oxides on the surface of the icy Saturn moons.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Astronomy \\& Astrophysics},\n\tauthor = {Ioppolo, S. and Kaňuchová, Z. and James, R. L. and Dawes, A. and Jones, N. C. and Hoffmann, S. V. and Mason, N. J. and Strazzulla, G.},\n\tmonth = sep,\n\tyear = {2020},\n\tpages = {A154},\n}\n\n

\n\n\n

\n \\textlessi\\textgreaterContext.\\textlessi/\\textgreater Molecular oxygen, nitrogen, and ozone have been detected on some satellites of Saturn and Jupiter, as well as on comets. They are also expected to be present in ice-grain mantles within star-forming regions. The continuous energetic processing of icy objects in the Solar System induces physical and chemical changes within the ice. Laboratory experiments that simulate energetic processing (ions, photons, and electrons) of ices are therefore essential for interpreting and directing future astronomical observations.\\textlessi\\textgreaterAims.\\textlessi/\\textgreater We provide vacuum ultraviolet (VUV) photoabsorption spectroscopic data of energetically processed nitrogen- and oxygen-rich ices that will help to identify absorption bands and/or spectral slopes observed on icy objects in the Solar System and on ice-grain mantles of the interstellar medium.\\textlessi\\textgreaterMethods.\\textlessi/\\textgreater We present VUV photoabsorption spectra of frozen O\\textlesssub\\textgreater2\\textlesssub/\\textgreater and N\\textlesssub\\textgreater2\\textlesssub/\\textgreater, a 1:1 mixture of both, and a new systematic set of pure and mixed nitrogen oxide ices. Spectra were obtained at 22 K before and after 1 keV electron bombardment of the ice sample. Ices were then annealed to higher temperatures to study their thermal evolution. In addition, Fourier-transform infrared spectroscopy was used as a secondary probe of molecular synthesis to better identify the physical and chemical processes at play.\\textlessi\\textgreaterResults.\\textlessi/\\textgreater Our VUV data show that ozone and the azide radical (N\\textlesssub\\textgreater3\\textlesssub/\\textgreater) are observed in our experiments after electron irradiation of pure O\\textlesssub\\textgreater2\\textlesssub/\\textgreater and N\\textlesssub\\textgreater2\\textlesssub/\\textgreater ices, respectively. Energetic processing of an O\\textlesssub\\textgreater2\\textlesssub/\\textgreater:N\\textlesssub\\textgreater2\\textlesssub/\\textgreater = 1:1 ice mixture leads to the formation of ozone along with a series of nitrogen oxides. The electron irradiation of solid nitrogen oxides, pure and in mixtures, induces the formation of new species such as O\\textlesssub\\textgreater2\\textlesssub/\\textgreater, N\\textlesssub\\textgreater2\\textlesssub/\\textgreater, and other nitrogen oxides not present in the initial ice. Results are discussed here in light of their relevance to various astrophysical environments. Finally, we show that VUV spectra of solid NO\\textlesssub\\textgreater2\\textlesssub/\\textgreater and water can reproduce the observational VUV profile of the cold surface of Enceladus, Dione, and Rhea, strongly suggesting the presence of nitrogen oxides on the surface of the icy Saturn moons.\n

\n\n\n

\n \n\n \n \n \n \n \n \n Mud flow levitation on Mars: Insights from laboratory simulations.\n \n \n \n \n\n\n \n Brož, P.; Krýza, O.; Conway, S. J.; Mueller, N. T.; Hauber, E.; Mazzini, A.; Raack, J.; Balme, M. R.; Sylvest, M. E.; and Patel, M. R.\n\n\n \n\n\n\n Earth and Planetary Science Letters, 545: 116406. September 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Mud$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{broz_mud_2020,\n\ttitle = {Mud flow levitation on {Mars}: {Insights} from laboratory simulations},\n\tvolume = {545},\n\tissn = {0012-821X},\n\tshorttitle = {Mud flow levitation on {Mars}},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0012821X20303502},\n\tdoi = {10.1016/j.epsl.2020.116406},\n\tabstract = {Sediment mobilisation occurring at depth and ultimately manifesting at the surface, is a process which may have operated on Mars. However, the propagation behaviour of this mixture of water and sediments (hereafter simply referred to as mud) over the martian surface, remains uncertain. Although most of the martian surface is below freezing today, locally warmer surface temperatures do occur, and our current knowledge suggests that similar conditions prevailed in the recent past. Here, we present the results of experiments performed inside a low pressure chamber to investigate mud propagation over a warm (∼295 K) unconsolidated sand surface under martian atmospheric pressure conditions (∼7 mbar). Results show that the mud boils while flowing over the warm surface. The gas released during this process can displace the underlying sand particles and hence erode part of the substrate. This “entrenched” flow can act as a platform for further mud propagation over the surface. The escaping gas causes intermittent levitation of the mud resulting in enhanced flow rates. The mud flow morphologies produced by these phenomena differ from those produced when mud flows over a frozen martian surface as well as from their terrestrial counterparts. The intense boiling removes the latent heat both from the mud and the subsurface, meaning that the mud flow would eventually start to freeze and hence changing again the way it propagates. The diverse morphology expressed by our experimental mudflows implies that caution should be exercised when interpreting flow features on the surface of Mars and other celestial bodies.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Earth and Planetary Science Letters},\n\tauthor = {Brož, P. and Krýza, O. and Conway, S. J. and Mueller, N. T. and Hauber, E. and Mazzini, A. and Raack, J. and Balme, M. R. and Sylvest, M. E. and Patel, M. R.},\n\tmonth = sep,\n\tyear = {2020},\n\tkeywords = {Mars, analogue experiments, levitation, low pressure chamber, mud flow, sedimentary volcanism},\n\tpages = {116406},\n}\n\n

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\n \n\n \n \n \n \n \n \n Mineralogy, chemistry, and composition of organic compounds in the fresh carbonaceous chondrite Mukundpura: CM1 or CM2?.\n \n \n \n \n\n\n \n Potin, S.; Beck, P.; Bonal, L.; Schmitt, B.; Garenne, A.; Moynier, F.; Agranier, A.; Schmitt-Kopplin, P.; Malik, A. K.; and Quirico, E.\n\n\n \n\n\n\n Meteoritics & Planetary Science, 55(7): 1681–1696. 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Mineralogy,$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{potin_mineralogy_2020,\n\ttitle = {Mineralogy, chemistry, and composition of organic compounds in the fresh carbonaceous chondrite {Mukundpura}: {CM1} or {CM2}?},\n\tvolume = {55},\n\tissn = {1945-5100},\n\tshorttitle = {Mineralogy, chemistry, and composition of organic compounds in the fresh carbonaceous chondrite {Mukundpura}},\n\turl = {https://onlinelibrary.wiley.com/doi/abs/10.1111/maps.13540},\n\tdoi = {10.1111/maps.13540},\n\tabstract = {We present here several laboratory analyses performed on the freshly fallen Mukundpura CM chondrite. Results of infrared transmission spectroscopy, thermogravimetry analysis, and reflectance spectroscopy show that Mukundpura is mainly composed of phyllosilicates. The rare earth trace elements composition and ultrahigh-resolution mass spectrometry of the soluble organic matter give results consistent with CM chondrites. Finally, Raman spectroscopy shows no signs of thermal alteration of the meteorite. All the results agree that Mukundpura has been strongly altered by water on its parent body. Comparison of the results obtained on the meteorite with those of other chondrites of known petrologic types leads to the conclusion that Mukundpura is similar to CM1 chondrites, which differ from its original classification as a CM2.},\n\tlanguage = {en},\n\tnumber = {7},\n\turldate = {2021-09-08},\n\tjournal = {Meteoritics \\& Planetary Science},\n\tauthor = {Potin, S. and Beck, P. and Bonal, L. and Schmitt, B. and Garenne, A. and Moynier, F. and Agranier, A. and Schmitt-Kopplin, P. and Malik, A. K. and Quirico, E.},\n\tyear = {2020},\n\tpages = {1681--1696},\n}\n\n

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\n \n\n \n \n \n \n \n \n An unusual compound object in Yamato 793408 (H3.2-an): The missing link between compound chondrules and macrochondrules?.\n \n \n \n \n\n\n \n Barosch, J.; Hezel, D. C.; Marrocchi, Y.; Gurenko, A.; and Lenting, C.\n\n\n \n\n\n\n Meteoritics & Planetary Science, 55(7): 1458–1470. 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"An$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{barosch_unusual_2020,\n\ttitle = {An unusual compound object in {Yamato} 793408 ({H3}.2-an): {The} missing link between compound chondrules and macrochondrules?},\n\tvolume = {55},\n\tissn = {1945-5100},\n\tshorttitle = {An unusual compound object in {Yamato} 793408 ({H3}.2-an)},\n\turl = {https://onlinelibrary.wiley.com/doi/abs/10.1111/maps.13496},\n\tdoi = {10.1111/maps.13496},\n\tabstract = {We found a large ( 2 mm) compound object in the primitive Yamato 793408 (H3.2-an) chondrite. It consists mostly of microcrystalline material, similar to chondrule mesostasis, that hosts an intact barred olivine (BO) chondrule. The object contains euhedral pyroxene and large individual olivine grains. Some olivine cores are indicative of refractory forsterites with very low Fe- and high Ca, Al-concentrations, although no 16O enrichment. The entire object is most likely a new and unique type, as no similar compound object has been described so far. We propose that it represents an intermediate stage between compound chondrules and macrochondrules, and formed from the collision between chondrules at low velocities (below 1 m s−1) at high temperatures (around 1550 °C). The macrochondrule also trapped and preserved a smaller BO chondrule. This object appears to be the first direct evidence for a genetic link between compound chondrules and macrochondrules. In accordance with previous suggestions and studies, compound chondrules and macrochondrules likely formed by the same mechanism of chondrule collisions, and each represents different formation conditions, such as ambient temperature and collision speed.},\n\tlanguage = {en},\n\tnumber = {7},\n\turldate = {2021-09-08},\n\tjournal = {Meteoritics \\& Planetary Science},\n\tauthor = {Barosch, Jens and Hezel, Dominik C. and Marrocchi, Yves and Gurenko, Andrey and Lenting, Christoph},\n\tyear = {2020},\n\tpages = {1458--1470},\n}\n\n

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\n \n\n \n \n \n \n \n \n Experimental evidence for lava-like mud flows under Martian surface conditions.\n \n \n \n \n\n\n \n Brož, P.; Krýza, O.; Wilson, L.; Conway, S. J.; Hauber, E.; Mazzini, A.; Raack, J.; Balme, M. R.; Sylvest, M. E.; and Patel, M. R.\n\n\n \n\n\n\n Nature Geoscience, 13(6): 403–407. June 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Experimental$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{broz_experimental_2020,\n\ttitle = {Experimental evidence for lava-like mud flows under {Martian} surface conditions},\n\tvolume = {13},\n\tcopyright = {2020 The Author(s), under exclusive licence to Springer Nature Limited},\n\tissn = {1752-0908},\n\turl = {https://www.nature.com/articles/s41561-020-0577-2},\n\tdoi = {10.1038/s41561-020-0577-2},\n\tabstract = {Large outflow channels on ancient terrains of Mars have been interpreted as the products of catastrophic flood events. The rapid burial of water-rich sediments after such flooding could have led to sedimentary volcanism, in which mixtures of sediment and water (mud) erupt to the surface. Tens of thousands of volcano-like landforms populate the northern lowlands and other local sedimentary depocentres on Mars. However, it is difficult to determine whether the edifices are related to igneous or mud extrusions, partly because the behaviour of extruded mud under Martian surface conditions is poorly constrained. Here we investigate the mechanisms of mud propagation on Mars using experiments performed inside a low-pressure chamber at cold temperatures. We found that low viscosity mud under Martian conditions propagates differently from that on Earth, because of a rapid freezing and the formation of an icy crust. Instead, the experimental mud flows propagate like terrestrial pahoehoe lava flows, with liquid mud spilling from ruptures in the frozen crust, and then refreezing to form a new flow lobe. We suggest that mud volcanism can explain the formation of some lava-like flow morphologies on Mars, and that similar processes may apply to cryovolcanic extrusions on icy bodies in the Solar System.},\n\tlanguage = {en},\n\tnumber = {6},\n\turldate = {2021-09-08},\n\tjournal = {Nature Geoscience},\n\tauthor = {Brož, Petr and Krýza, Ondřej and Wilson, Lionel and Conway, Susan J. and Hauber, Ernst and Mazzini, Adriano and Raack, Jan and Balme, Matthew R. and Sylvest, Matthew E. and Patel, Manish R.},\n\tmonth = jun,\n\tyear = {2020},\n\tpages = {403--407},\n}\n\n

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\n \n\n \n \n \n \n \n \n Organic Matter in the Solar System—Implications for Future on-Site and Sample Return Missions.\n \n \n \n \n\n\n \n Martins, Z.; Chan, Q. H. S.; Bonal, L.; King, A.; and Yabuta, H.\n\n\n \n\n\n\n Space Science Reviews, 216(4): 54. May 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Organic$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{martins_organic_2020,\n\ttitle = {Organic {Matter} in the {Solar} {System}—{Implications} for {Future} on-{Site} and {Sample} {Return} {Missions}},\n\tvolume = {216},\n\tissn = {1572-9672},\n\turl = {https://doi.org/10.1007/s11214-020-00679-6},\n\tdoi = {10.1007/s11214-020-00679-6},\n\tabstract = {Solar system bodies like comets, asteroids, meteorites and dust particles contain organic matter with different abundances, structures and chemical composition. This chapter compares the similarities and differences of the organic composition in these planetary bodies. Furthermore, these links are explored in the context of detecting the most pristine organic material, either by on-site analysis or sample return missions. Finally, we discuss the targets of potential future sample return missions, as well as the contamination controls that should be in place in order to successfully study pristine organic matter.},\n\tlanguage = {en},\n\tnumber = {4},\n\turldate = {2021-09-08},\n\tjournal = {Space Science Reviews},\n\tauthor = {Martins, Zita and Chan, Queenie Hoi Shan and Bonal, Lydie and King, Ashley and Yabuta, Hikaru},\n\tmonth = may,\n\tyear = {2020},\n\tpages = {54},\n}\n\n

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\n \n\n \n \n \n \n \n \n A model of the 3-μm hydration band with Exponentially Modified Gaussian (EMG) profiles: Application to hydrated chondrites and asteroids.\n \n \n \n \n\n\n \n Potin, S.; Manigand, S.; Beck, P.; Wolters, C.; and Schmitt, B.\n\n\n \n\n\n\n Icarus, 343: 113686. June 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"A$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{potin_model_2020,\n\ttitle = {A model of the 3-μm hydration band with {Exponentially} {Modified} {Gaussian} ({EMG}) profiles: {Application} to hydrated chondrites and asteroids},\n\tvolume = {343},\n\tissn = {0019-1035},\n\tshorttitle = {A model of the 3-μm hydration band with {Exponentially} {Modified} {Gaussian} ({EMG}) profiles},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0019103520300774},\n\tdoi = {10.1016/j.icarus.2020.113686},\n\tabstract = {We present here a new method to model the shape of the 3-μm absorption band in the reflectance spectra of meteorites and small bodies. The band is decomposed into several OH/H2O components using Exponentially Modified Gaussian (EMG) profiles, as well as possible organic components using Gaussian profiles when present. We compare this model to polynomial and multiple Gaussian profile fits and show that the EMGs model returns the best rendering of the shape of the band, with significantly lower residuals. We also propose as an example an algorithm to estimate the error on the band parameters using a bootstrap method. We then present an application of the model to two spectral analyses of smectites subjected to different H2O vapor pressures, and present the variations of the components with decreasing humidity. This example emphasizes the ability of this model to coherently retrieve weak bands that are hidden within much stronger ones.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Icarus},\n\tauthor = {Potin, S. and Manigand, S. and Beck, P. and Wolters, C. and Schmitt, B.},\n\tmonth = jun,\n\tyear = {2020},\n\tpages = {113686},\n}\n\n

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\n \n\n \n \n \n \n \n \n Diamond-Graphene Composite Nanostructures.\n \n \n \n \n\n\n \n Németh, P.; McColl, K.; Smith, R. L.; Murri, M.; Garvie, L. A. J.; Alvaro, M.; Pécz, B.; Jones, A. P.; Corà, F.; Salzmann, C. G.; and McMillan, P. F.\n\n\n \n\n\n\n Nano Letters, 20(5): 3611–3619. May 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Diamond-Graphene$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{nemeth_diamond-graphene_2020,\n\ttitle = {Diamond-{Graphene} {Composite} {Nanostructures}},\n\tvolume = {20},\n\tissn = {1530-6984},\n\turl = {https://doi.org/10.1021/acs.nanolett.0c00556},\n\tdoi = {10.1021/acs.nanolett.0c00556},\n\tabstract = {The search for new nanostructural topologies composed of elemental carbon is driven by technological opportunities as well as the need to understand the structure and evolution of carbon materials formed by planetary shock impact events and in laboratory syntheses. We describe two new families of diamond-graphene (diaphite) phases constructed from layered and bonded sp3 and sp2 nanostructural units and provide a framework for classifying the members of this new class of materials. The nanocomposite structures are identified within both natural impact diamonds and laboratory-shocked samples and possess diffraction features that have previously been assigned to lonsdaleite and postgraphite phases. The diaphite nanocomposites represent a new class of high-performance carbon materials that are predicted to combine the superhard qualities of diamond with high fracture toughness and ductility enabled by the graphitic units and the atomically defined interfaces between the sp3- and sp2-bonded nanodomains.},\n\tnumber = {5},\n\turldate = {2021-09-08},\n\tjournal = {Nano Letters},\n\tauthor = {Németh, Péter and McColl, Kit and Smith, Rachael L. and Murri, Mara and Garvie, Laurence A. J. and Alvaro, Matteo and Pécz, Béla and Jones, Adrian P. and Corà, Furio and Salzmann, Christoph G. and McMillan, Paul F.},\n\tmonth = may,\n\tyear = {2020},\n\tpages = {3611--3619},\n}\n\n

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\n \n\n \n \n \n \n \n \n Sectioning effects of porphyritic chondrules: Implications for the PP/POP/PO classification and correcting modal abundances of mineralogically zoned chondrules.\n \n \n \n \n\n\n \n Barosch, J.; Hezel, D. C.; Sawatzki, L.; Halbauer, L.; and Marrocchi, Y.\n\n\n \n\n\n\n Meteoritics & Planetary Science, 55(5): 993–999. 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Sectioning$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{barosch_sectioning_2020,\n\ttitle = {Sectioning effects of porphyritic chondrules: {Implications} for the {PP}/{POP}/{PO} classification and correcting modal abundances of mineralogically zoned chondrules},\n\tvolume = {55},\n\tissn = {1945-5100},\n\tshorttitle = {Sectioning effects of porphyritic chondrules},\n\turl = {https://onlinelibrary.wiley.com/doi/abs/10.1111/maps.13476},\n\tdoi = {10.1111/maps.13476},\n\tabstract = {Mineralogically zoned chondrules are a common chondrule type in chondrites. They consist of olivine cores, surrounded by low-Ca pyroxene rims. By serial sectioning porphyritic chondrules from carbonaceous, ordinary, and enstatite chondrites, we demonstrate that the 2-D textural appearances of these chondrules largely depend on where they are cut. The same chondrule may appear as a porphyritic pyroxene (PP) chondrule when sectioned through the low-Ca pyroxene rim, and as a porphyritic olivine-pyroxene (POP) or porphyritic olivine (PO) chondrule when sectioned close or through its equator. Chondrules previously classified into PP/POP/PO chondrules might therefore not represent different types, but various sections through mineralogically zoned chondrules. Classifying chondrule textures into PP, POP, and PO has therefore no unequivocal genetic meaning, it is merely descriptive. Sectioning effects further introduce a systematic bias when determining mineralogically zoned chondrule fractions from 2-D sections. We determined correction factors to estimate 3-D mineralogically zoned chondrule fractions when these have been determined in 2-D sections: 1.24 for carbonaceous chondrites, 1.29 for ordinary chondrites, and 1.62 for enstatite chondrites. Using these factors then shows that mineralogically zoned chondrules are the dominant chondrule type in chondrites with estimated 3-D fractions of 92\\% in CC, 52\\% in OC, and 46\\% in EC.},\n\tlanguage = {en},\n\tnumber = {5},\n\turldate = {2021-09-08},\n\tjournal = {Meteoritics \\& Planetary Science},\n\tauthor = {Barosch, Jens and Hezel, Dominik C. and Sawatzki, Lena and Halbauer, Lucia and Marrocchi, Yves},\n\tyear = {2020},\n\tpages = {993--999},\n}\n\n

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\n \n\n \n \n \n \n \n \n Fragmentation modelling of the 2019 August impact on Jupiter.\n \n \n \n \n\n\n \n Sankar, R.; Palotai, C.; Hueso, R.; Delcroix, M.; Chappel, E.; and Sánchez-Lavega, A.\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society, 493(4): 4622–4630. April 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Fragmentation$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{sankar_fragmentation_2020,\n\ttitle = {Fragmentation modelling of the 2019 {August} impact on {Jupiter}},\n\tvolume = {493},\n\tissn = {0035-8711},\n\turl = {https://doi.org/10.1093/mnras/staa563},\n\tdoi = {10.1093/mnras/staa563},\n\tabstract = {On 2019 August 7, an impact flash lasting ∼1 s was observed on Jupiter. The video of this event was analysed to obtain the light curve, and determine the energy release and initial mass. We find that the impactor released a total energy of 96–151 kilotons of TNT, corresponding to an initial mass between 190 and 260 metric tonnes with a diameter between 4 and 10 m. We developed a fragmentation model to simulate the atmospheric breakup of the object and reproduce the light curve. We model three different materials: cometary, stony, and metallic at speeds of 60, 65, and 70 km s−1, respectively, to determine the material make-up of the impacting object. The slower cases are best fitted by a strong, metallic object while the faster cases require a weaker material.},\n\tnumber = {4},\n\turldate = {2021-09-08},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {Sankar, Ramanakumar and Palotai, Csaba and Hueso, Ricardo and Delcroix, Marc and Chappel, Ethan and Sánchez-Lavega, Agustin},\n\tmonth = apr,\n\tyear = {2020},\n\tpages = {4622--4630},\n}\n\n

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\n \n\n \n \n \n \n \n \n Cosmic spherules from Widerøefjellet, Sør Rondane Mountains (East Antarctica).\n \n \n \n \n\n\n \n Goderis, S.; Soens, B.; Huber, M. S.; McKibbin, S.; van Ginneken, M.; Van Maldeghem, F.; Debaille, V.; Greenwood, R. C.; Franchi, I. A.; Cnudde, V.; Van Malderen, S.; Vanhaecke, F.; Koeberl, C.; Topa, D.; and Claeys, P.\n\n\n \n\n\n\n Geochimica et Cosmochimica Acta, 270: 112–143. February 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Cosmic$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{goderis_cosmic_2020,\n\ttitle = {Cosmic spherules from {Widerøefjellet}, {Sør} {Rondane} {Mountains} ({East} {Antarctica})},\n\tvolume = {270},\n\tissn = {0016-7037},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0016703719307240},\n\tdoi = {10.1016/j.gca.2019.11.016},\n\tabstract = {A newly discovered sedimentary accumulation of micrometeorites in the Sør Rondane Mountains of East Antarctica, close to the Widerøefjellet summit at ∼2750 m above sea level, is characterized in this work. The focus here lies on 2099 melted cosmic spherules larger than 200 μm, extracted from 3.2 kg of sampled sediment. Although the Widerøefjellet deposit shares similarities to the micrometeorite traps encountered in the Transantarctic Mountains, both subtle and more distinct differences in the physicochemical properties of the retrieved extraterrestrial particles and sedimentary host deposits are discernable (e.g., types of bedrock, degree of wind exposure, abundance of metal-rich particles). Unlike the Frontier Mountain and Miller Butte sedimentary traps, the size fraction below 240 μm indicates some degree of sorting at Widerøefjellet, potentially through the redistribution by wind, preferential alteration of smaller particles, or processing biases. However, the cosmic spherules larger than 300 μm appear largely unbiased following their size distribution, frequency by textural type, and bulk chemical compositions. Based on the available bedrock exposure ages for the Sør Rondane Mountains, extraterrestrial dust is estimated to have accumulated over a time span of ∼1–3 Ma at Widerøefjellet. Consequently, the Widerøefjellet collection reflects a substantial reservoir to sample the micrometeorite influx over this time interval. Petrographic observations and 3D microscopic CT imaging are combined with chemical and triple-oxygen isotopic analyses of silicate-rich cosmic spherules larger than 325 μm. The major element composition of 49 cosmic spherules confirms their principally chondritic parentage. For 18 glassy, 15 barred olivine, and 11 cryptocrystalline cosmic spherules, trace element concentrations are also reported on. Based on comparison with evaporation experiments reported in literature and accounting for siderophile and chalcophile element losses during high-density phase segregation and ejection, the observed compositional sequence largely reflects progressive heating and evaporation during atmospheric passage accompanied by significant redox shifts, although the influence of (refractory) chondrite mineral constituents and terrestrial alteration cannot be excluded in all cases. Twenty-eight cosmic spherules larger than 325 μm analyzed for triple-oxygen isotope ratios confirm inheritance from mostly carbonaceous chondritic precursor materials (∼55\\% of the particles). Yet, ∼30\\% of the measured cosmic spherules and ∼50\\% of all glassy cosmic spherules are characterized by oxygen isotope ratios above the terrestrial fractionation line, implying genetic links to ordinary chondrites and parent bodies currently unsampled by meteorites. The structural, textural, chemical, and isotopic characteristics of the cosmic spherules from the Sør Rondane Mountains, and particularly the high proportion of Mg-rich glass particles contained therein, imply a well-preserved and representative new sedimentary micrometeorite collection from a previously unstudied region in East Antarctica characterized by distinct geological and exposure histories.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Geochimica et Cosmochimica Acta},\n\tauthor = {Goderis, Steven and Soens, Bastien and Huber, Matthew S. and McKibbin, Seann and van Ginneken, Matthias and Van Maldeghem, Flore and Debaille, Vinciane and Greenwood, Richard C. and Franchi, Ian A. and Cnudde, Veerle and Van Malderen, Stijn and Vanhaecke, Frank and Koeberl, Christian and Topa, Dan and Claeys, Philippe},\n\tmonth = feb,\n\tyear = {2020},\n\tkeywords = {Atmospheric heating, Cosmic spherules, Extraterrestrial dust, Oxygen isotope ratios, Parent bodies},\n\tpages = {112--143},\n}\n\n

\n\n\n

\n A newly discovered sedimentary accumulation of micrometeorites in the Sør Rondane Mountains of East Antarctica, close to the Widerøefjellet summit at ∼2750 m above sea level, is characterized in this work. The focus here lies on 2099 melted cosmic spherules larger than 200 μm, extracted from 3.2 kg of sampled sediment. Although the Widerøefjellet deposit shares similarities to the micrometeorite traps encountered in the Transantarctic Mountains, both subtle and more distinct differences in the physicochemical properties of the retrieved extraterrestrial particles and sedimentary host deposits are discernable (e.g., types of bedrock, degree of wind exposure, abundance of metal-rich particles). Unlike the Frontier Mountain and Miller Butte sedimentary traps, the size fraction below 240 μm indicates some degree of sorting at Widerøefjellet, potentially through the redistribution by wind, preferential alteration of smaller particles, or processing biases. However, the cosmic spherules larger than 300 μm appear largely unbiased following their size distribution, frequency by textural type, and bulk chemical compositions. Based on the available bedrock exposure ages for the Sør Rondane Mountains, extraterrestrial dust is estimated to have accumulated over a time span of ∼1–3 Ma at Widerøefjellet. Consequently, the Widerøefjellet collection reflects a substantial reservoir to sample the micrometeorite influx over this time interval. Petrographic observations and 3D microscopic CT imaging are combined with chemical and triple-oxygen isotopic analyses of silicate-rich cosmic spherules larger than 325 μm. The major element composition of 49 cosmic spherules confirms their principally chondritic parentage. For 18 glassy, 15 barred olivine, and 11 cryptocrystalline cosmic spherules, trace element concentrations are also reported on. Based on comparison with evaporation experiments reported in literature and accounting for siderophile and chalcophile element losses during high-density phase segregation and ejection, the observed compositional sequence largely reflects progressive heating and evaporation during atmospheric passage accompanied by significant redox shifts, although the influence of (refractory) chondrite mineral constituents and terrestrial alteration cannot be excluded in all cases. Twenty-eight cosmic spherules larger than 325 μm analyzed for triple-oxygen isotope ratios confirm inheritance from mostly carbonaceous chondritic precursor materials (∼55% of the particles). Yet, ∼30% of the measured cosmic spherules and ∼50% of all glassy cosmic spherules are characterized by oxygen isotope ratios above the terrestrial fractionation line, implying genetic links to ordinary chondrites and parent bodies currently unsampled by meteorites. The structural, textural, chemical, and isotopic characteristics of the cosmic spherules from the Sør Rondane Mountains, and particularly the high proportion of Mg-rich glass particles contained therein, imply a well-preserved and representative new sedimentary micrometeorite collection from a previously unstudied region in East Antarctica characterized by distinct geological and exposure histories.\n

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\n \n\n \n \n \n \n \n \n Radiogenic isotopic and clay mineralogical signatures of terrigenous particles as water-mass tracers: New insights into South Atlantic deep circulation during the last termination.\n \n \n \n \n\n\n \n Beny, F.; Bout-Roumazeilles, V.; Davies, G. R.; Waelbroeck, C.; Bory, A.; Tribovillard, N.; Delattre, M.; and Abraham, R.\n\n\n \n\n\n\n Quaternary Science Reviews, 228: 106089. January 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Radiogenic$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{beny_radiogenic_2020,\n\ttitle = {Radiogenic isotopic and clay mineralogical signatures of terrigenous particles as water-mass tracers: {New} insights into {South} {Atlantic} deep circulation during the last termination},\n\tvolume = {228},\n\tissn = {0277-3791},\n\tshorttitle = {Radiogenic isotopic and clay mineralogical signatures of terrigenous particles as water-mass tracers},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0277379119305955},\n\tdoi = {10.1016/j.quascirev.2019.106089},\n\tabstract = {The past evolution of the Southern Ocean, one of the major components of the climatic system, is still a matter of debate. This study provides new insights into the deep Southern Ocean circulation based on the radiogenic isotopes and clay mineralogical signature of the terrigenous fractions transported by the main deep water masses to sediments recovered in core MD07-3076Q from the central South Atlantic. This approach successfully permits: (1) provenance identification of the various grain-size fractions (clay, cohesive silt and sortable silt); (2) assignment of each grain-size fraction to a specific water-mass; (3) reconstruction of past changes in the main deep water-mass pathways. These data document the evolution of deep-water masses in the South Atlantic Ocean during the last deglaciation. The Antarctic Bottom Water (AABW) speed and northward extension were maximum at the end of the Last Glacial Maximum (LGM), associated with strong bottom water production in the Weddell Sea, together with a vigorous Lower Circumpolar Deep Water (LCDW). In contrast the North Atlantic Deep Water (NADW) circulation was weaker than today. The onset of the deglaciation (from 17.5 ka to 15 ka, ∼Heinrich Stadial 1, HS 1) was marked by weakening and southerly retreat of the AABW and by an increase of mixing between AABW and LCDW. The speed of the AABW remained at its lowest during the Bølling Allerød (B/A) and the Younger Dryas (YD), and the LCDW slowed and retreated to the south, while the NADW progressively migrated southward, deepened, and strengthened between the beginning of the Bølling Allerød and the Holocene (from ∼15 to 10 ka).},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Quaternary Science Reviews},\n\tauthor = {Beny, F. and Bout-Roumazeilles, V. and Davies, G. R. and Waelbroeck, C. and Bory, A. and Tribovillard, N. and Delattre, M. and Abraham, R.},\n\tmonth = jan,\n\tyear = {2020},\n\tkeywords = {Clay mineralogy, Grain size distribution, Last deglaciation, Paleoceanography, Radiogenic isotopes, South Atlantic, Southern Ocean},\n\tpages = {106089},\n}\n\n

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\n \n\n \n \n \n \n \n \n Saturn atmospheric dynamics one year after Cassini: Long-lived features and time variations in the drift of the Hexagon.\n \n \n \n \n\n\n \n Hueso, R.; Sánchez-Lavega, A.; Rojas, J. F.; Simon, A. A.; Barry, T.; Río-Gaztelurrutia, T. d.; Antuñano, A.; Sayanagi, K. M.; Delcroix, M.; Fletcher, L. N.; García-Melendo, E.; Pérez-Hoyos, S.; Blalock, J.; Colas, F.; Gómez-Forrellad, J. M.; Gunnarson, J. L.; Peach, D.; and Wong, M. H.\n\n\n \n\n\n\n Icarus, 336: 113429. January 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Saturn$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{hueso_saturn_2020,\n\ttitle = {Saturn atmospheric dynamics one year after {Cassini}: {Long}-lived features and time variations in the drift of the {Hexagon}},\n\tvolume = {336},\n\tissn = {0019-1035},\n\tshorttitle = {Saturn atmospheric dynamics one year after {Cassini}},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0019103519301861},\n\tdoi = {10.1016/j.icarus.2019.113429},\n\tabstract = {We examine Saturn's atmospheric dynamics with observations in the visible range from ground-based telescopes and Hubble Space Telescope (HST). We present a detailed analysis of observations acquired during 2018 obtaining drift rates of major meteorological systems from the equator to the north polar hexagon. A system of polar storms that appeared in the planet in March 2018 and remained active with a complex phenomenology at least until September is analyzed elsewhere (Sánchez-Lavega et al., 2019). Many of the regular cloud features visible in 2018 are long-lived and can be identified in Saturn images in 2017, and in some cases, for up to a decade using also Cassini ISS images. Without considering the polar storms, the most interesting long-lived cloud systems are: i) A bright white spot in the Equatorial Zone that can be tracked continuously since 2014 with minimal changes in its zonal velocity, which was 444.3 ± 3.1 m s−1 in 2014 and 452.4 ± 1.7 m s−1 in 2018. This velocity is remarkably different from the zonal winds at the cloud level at its latitude during the Cassini mission, and is closer to zonal winds obtained at the time of the Voyagers flybys and to zonal winds from Cassini VIMS infrared images of the lower atmosphere. ii) A large long-lived Anticyclone Vortex, here AV, that formed after the Great White Spot of 2010–2011. This vortex has changed significantly in visual contrast, drift rate and latitude with minor changes in size over the last years. iii) A system of subpolar vortices at latitudes 60–65°N present at least since 2011. These vortices and additional atmospheric features here studied follow drift rates consistent with zonal winds obtained by Cassini. We also present a study of the positions of the vertices of Saturn's north polar hexagon from 2015 to 2018. These measurements are compared with previous analyses during the Cassini mission (2007–2014), observations with HST in the 90s, and data from the Voyagers in 1980–1981 to explore the long-term variability of the hexagon's drift rate. We find variations in the drift rate of the hexagon through these epochs that can not be fit by seasonal changes in the polar area. Instead, the different drift rates reinforce the role of the North Polar Spot that was present in the Voyager epoch and in the early 90s to cause a faster drift rate of the hexagon at that time compared with the current slower one.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Icarus},\n\tauthor = {Hueso, R. and Sánchez-Lavega, A. and Rojas, J. F. and Simon, A. A. and Barry, T. and Río-Gaztelurrutia, T. del and Antuñano, A. and Sayanagi, K. M. and Delcroix, M. and Fletcher, L. N. and García-Melendo, E. and Pérez-Hoyos, S. and Blalock, J. and Colas, F. and Gómez-Forrellad, J. M. and Gunnarson, J. L. and Peach, D. and Wong, M. H.},\n\tmonth = jan,\n\tyear = {2020},\n\tkeywords = {Atmosphere, Atmospheres, Dynamics, Saturn},\n\tpages = {113429},\n}\n\n

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\n We examine Saturn's atmospheric dynamics with observations in the visible range from ground-based telescopes and Hubble Space Telescope (HST). We present a detailed analysis of observations acquired during 2018 obtaining drift rates of major meteorological systems from the equator to the north polar hexagon. A system of polar storms that appeared in the planet in March 2018 and remained active with a complex phenomenology at least until September is analyzed elsewhere (Sánchez-Lavega et al., 2019). Many of the regular cloud features visible in 2018 are long-lived and can be identified in Saturn images in 2017, and in some cases, for up to a decade using also Cassini ISS images. Without considering the polar storms, the most interesting long-lived cloud systems are: i) A bright white spot in the Equatorial Zone that can be tracked continuously since 2014 with minimal changes in its zonal velocity, which was 444.3 ± 3.1 m s−1 in 2014 and 452.4 ± 1.7 m s−1 in 2018. This velocity is remarkably different from the zonal winds at the cloud level at its latitude during the Cassini mission, and is closer to zonal winds obtained at the time of the Voyagers flybys and to zonal winds from Cassini VIMS infrared images of the lower atmosphere. ii) A large long-lived Anticyclone Vortex, here AV, that formed after the Great White Spot of 2010–2011. This vortex has changed significantly in visual contrast, drift rate and latitude with minor changes in size over the last years. iii) A system of subpolar vortices at latitudes 60–65°N present at least since 2011. These vortices and additional atmospheric features here studied follow drift rates consistent with zonal winds obtained by Cassini. We also present a study of the positions of the vertices of Saturn's north polar hexagon from 2015 to 2018. These measurements are compared with previous analyses during the Cassini mission (2007–2014), observations with HST in the 90s, and data from the Voyagers in 1980–1981 to explore the long-term variability of the hexagon's drift rate. We find variations in the drift rate of the hexagon through these epochs that can not be fit by seasonal changes in the polar area. Instead, the different drift rates reinforce the role of the North Polar Spot that was present in the Voyager epoch and in the early 90s to cause a faster drift rate of the hexagon at that time compared with the current slower one.\n

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\n \n\n \n \n \n \n \n \n Virtual European Solar & Planetary Access (VESPA): A Planetary Science Virtual Observatory Cornerstone.\n \n \n \n \n\n\n \n Erard, S.; Cecconi, B.; Sidaner, P. L.; Chauvin, C.; Rossi, A. P.; Minin, M.; Capria, T.; Ivanovski, S.; Schmitt, B.; Génot, V.; André, N.; Marmo, C.; Vandaele, A. C.; Trompet, L.; Scherf, M.; Hueso, R.; Määttänen, A.; Carry, B.; Achilleos, N.; Soucek, J.; Pisa, D.; Benson, K.; Fernique, P.; and Millour, E.\n\n\n \n\n\n\n Data Science Journal, 19(1): 22. May 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Virtual$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n\n\n\n

@article{erard_virtual_2020,\n\ttitle = {Virtual {European} {Solar} \\& {Planetary} {Access} ({VESPA}): {A} {Planetary} {Science} {Virtual} {Observatory} {Cornerstone}},\n\tvolume = {19},\n\tcopyright = {Authors who publish with this journal agree to the following terms:    Authors retain copyright and grant the journal right of first publication with the work simultaneously licensed under a  Creative Commons Attribution License  that allows others to share the work with an acknowledgement of the work's authorship and initial publication in this journal.  Authors are able to enter into separate, additional contractual arrangements for the non-exclusive distribution of the journal's published version of the work (e.g., post it to an institutional repository or publish it in a book), with an acknowledgement of its initial publication in this journal.  Authors are permitted and encouraged to post their work online (e.g., in institutional repositories or on their website) prior to and during the submission process, as it can lead to productive exchanges, as well as earlier and greater citation of published work (See  The Effect of Open Access ).  All third-party images reproduced on this journal are shared under Educational Fair Use. For more information on  Educational Fair Use , please see  this useful checklist prepared by Columbia University Libraries .   All copyright  of third-party content posted here for research purposes belongs to its original owners.  Unless otherwise stated all references to characters and comic art presented on this journal are ©, ® or ™ of their respective owners. No challenge to any owner’s rights is intended or should be inferred.},\n\tissn = {1683-1470},\n\tshorttitle = {Virtual {European} {Solar} \\& {Planetary} {Access} ({VESPA})},\n\turl = {http://datascience.codata.org/articles/10.5334/dsj-2020-022/},\n\tdoi = {10.5334/dsj-2020-022},\n\tabstract = {The Europlanet-2020 programme, which ended on Aug 31st, 2019, included an activity called VESPA (Virtual European Solar and Planetary Access), which focused on adapting Virtual Observatory (VO) techniques to handle Planetary Science data. This paper describes some aspects of VESPA at the end of this 4-years development phase and at the onset of the newly selected Europlanet-2024 programme starting in 2020. The main objectives of VESPA are to facilitate searches both in big archives and in small databases, to enable data analysis by providing simple data access and online visualization functions, and to allow research teams to publish derived data in an interoperable environment as easily as possible. VESPA encompasses a wide scope, including surfaces, atmospheres, magnetospheres and planetary plasmas, small bodies, heliophysics, exoplanets, and spectroscopy in solid phase. This system relies in particular on standards and tools developed for the Astronomy VO (IVOA) and extends them where required to handle specificities of Solar System studies. It also aims at making the VO compatible with tools and protocols developed in different contexts, for instance GIS for planetary surfaces, or time series tools for plasma-related measurements. An essential part of the activity is to publish a significant amount of high-quality data in this system, with a focus on derived products resulting from data analysis or simulations.},\n\tlanguage = {en},\n\tnumber = {1},\n\turldate = {2021-09-08},\n\tjournal = {Data Science Journal},\n\tauthor = {Erard, S. and Cecconi, B. and Sidaner, P. Le and Chauvin, C. and Rossi, A. P. and Minin, M. and Capria, T. and Ivanovski, S. and Schmitt, B. and Génot, V. and André, N. and Marmo, C. and Vandaele, A. C. and Trompet, L. and Scherf, M. and Hueso, R. and Määttänen, A. and Carry, B. and Achilleos, N. and Soucek, J. and Pisa, D. and Benson, K. and Fernique, P. and Millour, E.},\n\tmonth = may,\n\tyear = {2020},\n\tkeywords = {GIS, Solar System, Virtual Observatory},\n\tpages = {22},\n}\n\n

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\n \n\n \n \n \n \n \n \n THE IMPORTANCE OF GROUND-BASED AND SATELLITE OBSERVATIONS FOR MONITORING AND ESTIMATION OF UV RADIATION IN NOVI SAD (SERBIA).\n \n \n \n \n\n\n \n \n\n\n \n\n\n\n Зборник радова Географског института \"Јован Цвијић\" САНУ, 70(1): 57–70. 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"THE$ Paper\n \n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{noauthor_importance_2020,\n\ttitle = {{THE} {IMPORTANCE} {OF} {GROUND}-{BASED} {AND} {SATELLITE} {OBSERVATIONS} {FOR} {MONITORING} {AND} {ESTIMATION} {OF} {UV} {RADIATION} {IN} {NOVI} {SAD} ({SERBIA})},\n\tvolume = {70},\n\tissn = {0350-7599, 1821-2808},\n\turl = {https://www.ceeol.com/search/article-detail?id=897512},\n\tlanguage = {English},\n\tnumber = {1},\n\turldate = {2021-09-08},\n\tjournal = {Зборник радова Географског института "Јован Цвијић" САНУ},\n\tyear = {2020},\n\tpages = {57--70},\n}\n\n

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\n \n\n \n \n \n \n \n \n The challenges in hypervelocity microphysics research on meteoroid impacts into the atmosphere.\n \n \n \n \n\n\n \n Vinkovic, D.; and Gritsevich, M.\n\n\n \n\n\n\n Zbornik radova - Geografski institut \"Jovan Cvijić\", 70(1): 45–55. 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"The$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{vinkovic_challenges_2020,\n\ttitle = {The challenges in hypervelocity microphysics research on meteoroid impacts into the atmosphere},\n\tvolume = {70},\n\tissn = {0350-7599},\n\turl = {https://researchportal.helsinki.fi/en/publications/the-challenges-in-hypervelocity-microphysics-research-on-meteoroi},\n\tdoi = {10.2298/IJGI2001045V},\n\tlanguage = {English},\n\tnumber = {1},\n\turldate = {2021-09-08},\n\tjournal = {Zbornik radova - Geografski institut "Jovan Cvijić"},\n\tauthor = {Vinkovic, Dejan and Gritsevich, Maria},\n\tyear = {2020},\n\tpages = {45--55},\n}\n\n

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\n \n\n \n \n \n \n \n \n MASER: A Science Ready Toolbox for Low Frequency Radio Astronomy.\n \n \n \n \n\n\n \n Cecconi, B.; Loh, A.; Sidaner, P. L.; Savalle, R.; Bonnin, X.; Nguyen, Q. N.; Lion, S.; Shih, A.; Aicardi, S.; Zarka, P.; Louis, C.; Coffre, A.; Lamy, L.; Denis, L.; Grießmeier, J.; Faden, J.; Piker, C.; André, N.; Génot, V.; Erard, S.; Mafi, J. N.; King, T. A.; Sky, J.; and Demleitner, M.\n\n\n \n\n\n\n Data Science Journal, 19(1): 12. March 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"MASER:$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n\n\n\n

@article{cecconi_maser_2020,\n\ttitle = {{MASER}: {A} {Science} {Ready} {Toolbox} for {Low} {Frequency} {Radio} {Astronomy}},\n\tvolume = {19},\n\tcopyright = {Authors who publish with this journal agree to the following terms:    Authors retain copyright and grant the journal right of first publication with the work simultaneously licensed under a  Creative Commons Attribution License  that allows others to share the work with an acknowledgement of the work's authorship and initial publication in this journal.  Authors are able to enter into separate, additional contractual arrangements for the non-exclusive distribution of the journal's published version of the work (e.g., post it to an institutional repository or publish it in a book), with an acknowledgement of its initial publication in this journal.  Authors are permitted and encouraged to post their work online (e.g., in institutional repositories or on their website) prior to and during the submission process, as it can lead to productive exchanges, as well as earlier and greater citation of published work (See  The Effect of Open Access ).  All third-party images reproduced on this journal are shared under Educational Fair Use. For more information on  Educational Fair Use , please see  this useful checklist prepared by Columbia University Libraries .   All copyright  of third-party content posted here for research purposes belongs to its original owners.  Unless otherwise stated all references to characters and comic art presented on this journal are ©, ® or ™ of their respective owners. No challenge to any owner’s rights is intended or should be inferred.},\n\tissn = {1683-1470},\n\tshorttitle = {{MASER}},\n\turl = {http://datascience.codata.org/articles/10.5334/dsj-2020-012/},\n\tdoi = {10.5334/dsj-2020-012},\n\tabstract = {MASER (Measurements, Analysis, and Simulation of Emission in the Radio range) is a comprehensive infrastructure dedicated to time-dependent low frequency radio astronomy (up to about 50 MHz). The main radio sources observed in this spectral range are the Sun, the magnetized planets (Earth, Jupiter, Saturn), and our Galaxy, which are observed either from ground or space. Ground observatories can capture high resolution data streams with a high sensitivity. Conversely, space-borne instruments can observe below the ionospheric cut-off (at about 10 MHz) and can be placed closer to the studied object. Several tools have been developed in the last decade for sharing space physics data. Data visualization tools developed by various institutes are available to share, display and analyse space physics time series and spectrograms. The MASER team has selected a sub-set of those tools and applied them to low frequency radio astronomy. MASER also includes a Python software library for reading raw data from agency archives.},\n\tlanguage = {en},\n\tnumber = {1},\n\turldate = {2021-09-08},\n\tjournal = {Data Science Journal},\n\tauthor = {Cecconi, Baptiste and Loh, Alan and Sidaner, Pierre Le and Savalle, Renaud and Bonnin, Xavier and Nguyen, Quynh Nhu and Lion, Sonny and Shih, Albert and Aicardi, Stéphane and Zarka, Philippe and Louis, Corentin and Coffre, Andrée and Lamy, Laurent and Denis, Laurent and Grießmeier, Jean-Mathias and Faden, Jeremy and Piker, Chris and André, Nicolas and Génot, Vincent and Erard, Stéphane and Mafi, Joseph N. and King, Todd A. and Sky, Jim and Demleitner, Markus},\n\tmonth = mar,\n\tyear = {2020},\n\tkeywords = {Interoperability, Radio astronomy, Tools},\n\tpages = {12},\n}\n\n

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\n \n\n \n \n \n \n \n \n Primordial formation of major silicates in a protoplanetary disc with homogeneous 26Al/27Al.\n \n \n \n \n\n\n \n Gregory, T.; Luu, T.; Coath, C. D.; Russell, S. S.; and Elliott, T.\n\n\n \n\n\n\n Science Advances. March 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Primordial$ Paper\n \n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{gregory_primordial_2020,\n\ttitle = {Primordial formation of major silicates in a protoplanetary disc with homogeneous {26Al}/{27Al}},\n\tcopyright = {Copyright © 2020 The Authors, some rights reserved; exclusive licensee American Association for the Advancement of Science. No claim to original U.S. Government Works. Distributed under a Creative Commons Attribution NonCommercial License 4.0 (CC BY-NC).},\n\turl = {https://www.science.org/doi/abs/10.1126/sciadv.aay9626},\n\tabstract = {Primordial refractory silicates record evidence that aluminum-26 was efficiently mixed across different solar system sources.},\n\tlanguage = {EN},\n\turldate = {2021-09-08},\n\tjournal = {Science Advances},\n\tauthor = {Gregory, Timothy and Luu, Tu-Han and Coath, Christopher D. and Russell, Sara S. and Elliott, Tim},\n\tmonth = mar,\n\tyear = {2020},\n}\n\n

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\n \n\n \n \n \n \n \n The Search for Organic Signatures Within Dynamic Features on the Martian Surface.\n \n \n \n\n\n \n Campbell, J. D.; Schmitt, B.; Brissaud, O.; and Muller, J.\n\n\n \n\n\n\n In Oxford, UK, January 2020. \n \n\n\n\n
\n\n\n\n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@inproceedings{campbell_search_2020,\n\taddress = {Oxford, UK},\n\ttitle = {The {Search} for {Organic} {Signatures} {Within} {Dynamic} {Features} on the {Martian} {Surface}},\n\tauthor = {Campbell, J. D. and Schmitt, B. and Brissaud, O. and Muller, J.-P.},\n\tmonth = jan,\n\tyear = {2020},\n}\n\n

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\n \n\n \n \n \n \n \n \n Hyperspectral Mapping of the Martian South Polar Residual Cap Using Laboratory Analogues and Orbital Imagery.\n \n \n \n \n\n\n \n Campbell, J. D.; Schmitt, B.; Brissaud, O.; and Muller, J. -.\n\n\n \n\n\n\n LPI Contributions, 2099: 6021. January 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Hyperspectral$ Paper\n \n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{campbell_hyperspectral_2020,\n\ttitle = {Hyperspectral {Mapping} of the {Martian} {South} {Polar} {Residual} {Cap} {Using} {Laboratory} {Analogues} and {Orbital} {Imagery}},\n\tvolume = {2099},\n\tissn = {0161-5297},\n\turl = {https://ui.adsabs.harvard.edu/abs/2020LPICo2099.6021C},\n\tabstract = {In this work, we show the results of laboratory experiments designed to establish diagnostic spectra of organic signatures CO2 ice, and apply the data to orbital hyperspectral imagery to look at dust composition and changes over time.},\n\turldate = {2021-07-26},\n\tjournal = {LPI Contributions},\n\tauthor = {Campbell, J. D. and Schmitt, B. and Brissaud, O. and Muller, J. -P.},\n\tmonth = jan,\n\tyear = {2020},\n\tpages = {6021},\n}\n\n

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\n \n\n \n \n \n \n \n \n Detection of Polycyclic Aromatic Hydrocarbons in Mars Analogues.\n \n \n \n \n\n\n \n Campbell, J. D.; Schmitt, B.; Brissaud, O.; and Muller, J. -.\n\n\n \n\n\n\n ,1928. March 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Detection$ Paper\n \n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{campbell_detection_2020,\n\ttitle = {Detection of {Polycyclic} {Aromatic} {Hydrocarbons} in {Mars} {Analogues}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2020LPI....51.1928C},\n\tabstract = {A series of laboratory experiments carried out to generate diagnostic infrared spectra for Polycyclic Aromatic Hydrocarbons of astrobiological interest.},\n\turldate = {2021-07-26},\n\tauthor = {Campbell, J. D. and Schmitt, B. and Brissaud, O. and Muller, J. -P.},\n\tmonth = mar,\n\tyear = {2020},\n\tpages = {1928},\n}\n\n

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\n \n 2019\n \n \n (16)\n \n \n

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\n \n\n \n \n \n \n \n \n Lipid Biomarker and Carbon Stable Isotope Survey on the Dallol Hydrothermal System in Ethiopia.\n \n \n \n \n\n\n \n Carrizo, D.; Sánchez-García, L.; Rodriguez, N.; and Gómez, F.\n\n\n \n\n\n\n Astrobiology, 19: 1474–1489. December 2019.\n ADS Bibcode: 2019AsBio..19.1474C\n\n\n\n
\n\n\n\n \n \n $\"Lipid$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n\n\n\n

@article{2019AsBio..19.1474C,\n\ttitle = {Lipid {Biomarker} and {Carbon} {Stable} {Isotope} {Survey} on the {Dallol} {Hydrothermal} {System} in {Ethiopia}},\n\tvolume = {19},\n\tissn = {1531-1074},\n\turl = {https://ui.adsabs.harvard.edu/abs/2019AsBio..19.1474C},\n\tdoi = {10.1089/ast.2018.1963},\n\tabstract = {The remote Dallol Hot Springs, an active hydrothermal system in the volcanic region of Danakil (Ethiopia), is an interesting yet poorly studied polyextreme environment for investigating the limits of life. Here, we explored the presence of signs of life in five samples of sinter deposits at Dallol, by means of lipid biomarkers and stable isotope composition. The results reveal the existence of biological material with predominance of (presently or recently active) microbial sources, according to the relative abundance of low-over-high molecular weight moieties (n-alkanes, n-carboxylic acids, or n-alkanols), and the detection of diverse microbial-diagnostic compounds (i.e., monomethyl alkanes; C16:1 ω7, C18:1 ω9, C18:1 ω10, C18:2 ω6,9 and iso/anteiso C15 and C17 carboxylic acids; or short-chained dicarboxylic acids). The molecular lipid patterns at Dallol suggest a microbial community largely composed of thermophilic members of the Aquificae, Thermotogae, Chroroflexi, or Proteobacteria phyla, as well as microbial consortia of phototrophs (e.g., Cyanobacteria-Chloroflexi) in lower-temperature and higher-pH niches. Autotrophic sources most likely using the Calvin cycle, together with the acetyl coenzyme A (CoA) pathway, were inferred from the depleted bulk δ13C ratios (-25.9/-22.6‰), while sulfate-reducing bacteria were considered according to enriched sulfate (7.3/11.7‰) and total sulfur (20.5/8.2‰) δ34S ratios. The abundance of functionalized hydrocarbons (i.e., n-carboxylic acids and n-alkanols) and the distinct even-over-odd predominance/preference on the typically odd n-alkanes (CPIalkanes ≤ 1) pointed to active or recent microbial metabolisms. This study documents the detection of biosignatures in the polyextreme environment of Dallol and raises the possibility of finding life or its remnants in other remote locations on Earth, where the harsh environmental conditions would lead to expect otherwise. These findings are relevant for understanding the limits of life and have implications for searching for hypothetical life vestiges in extreme environments beyond Earth.},\n\turldate = {2021-09-08},\n\tjournal = {Astrobiology},\n\tauthor = {Carrizo, Daniel and Sánchez-García, Laura and Rodriguez, Nuria and Gómez, Felipe},\n\tmonth = dec,\n\tyear = {2019},\n\tnote = {ADS Bibcode: 2019AsBio..19.1474C},\n\tkeywords = {Research Articles},\n\tpages = {1474--1489},\n}\n\n

\n\n\n

\n The remote Dallol Hot Springs, an active hydrothermal system in the volcanic region of Danakil (Ethiopia), is an interesting yet poorly studied polyextreme environment for investigating the limits of life. Here, we explored the presence of signs of life in five samples of sinter deposits at Dallol, by means of lipid biomarkers and stable isotope composition. The results reveal the existence of biological material with predominance of (presently or recently active) microbial sources, according to the relative abundance of low-over-high molecular weight moieties (n-alkanes, n-carboxylic acids, or n-alkanols), and the detection of diverse microbial-diagnostic compounds (i.e., monomethyl alkanes; C16:1 ω7, C18:1 ω9, C18:1 ω10, C18:2 ω6,9 and iso/anteiso C15 and C17 carboxylic acids; or short-chained dicarboxylic acids). The molecular lipid patterns at Dallol suggest a microbial community largely composed of thermophilic members of the Aquificae, Thermotogae, Chroroflexi, or Proteobacteria phyla, as well as microbial consortia of phototrophs (e.g., Cyanobacteria-Chloroflexi) in lower-temperature and higher-pH niches. Autotrophic sources most likely using the Calvin cycle, together with the acetyl coenzyme A (CoA) pathway, were inferred from the depleted bulk δ13C ratios (-25.9/-22.6‰), while sulfate-reducing bacteria were considered according to enriched sulfate (7.3/11.7‰) and total sulfur (20.5/8.2‰) δ34S ratios. The abundance of functionalized hydrocarbons (i.e., n-carboxylic acids and n-alkanols) and the distinct even-over-odd predominance/preference on the typically odd n-alkanes (CPIalkanes ≤ 1) pointed to active or recent microbial metabolisms. This study documents the detection of biosignatures in the polyextreme environment of Dallol and raises the possibility of finding life or its remnants in other remote locations on Earth, where the harsh environmental conditions would lead to expect otherwise. These findings are relevant for understanding the limits of life and have implications for searching for hypothetical life vestiges in extreme environments beyond Earth.\n

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\n \n\n \n \n \n \n \n \n Ancient recycled lower crust in the mantle source of recent Italian magmatism.\n \n \n \n \n\n\n \n Koornneef, J. M.; Nikogosian, I.; van Bergen, M. J.; Vroon, P. Z.; and Davies, G. R.\n\n\n \n\n\n\n Nature Communications, 10(1): 3237. July 2019.\n \n\n\n\n
\n\n\n\n \n \n $\"Ancient$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{koornneef_ancient_2019,\n\ttitle = {Ancient recycled lower crust in the mantle source of recent {Italian} magmatism},\n\tvolume = {10},\n\tcopyright = {2019 The Author(s)},\n\tissn = {2041-1723},\n\turl = {https://www.nature.com/articles/s41467-019-11072-5},\n\tdoi = {10.1038/s41467-019-11072-5},\n\tabstract = {Recycling of Earth’s crust through subduction and delamination contributes to mantle heterogeneity. Melt inclusions in early crystallised magmatic minerals record greater geochemical variability than host lavas and more fully reflect the heterogeneity of magma sources. To date, use of multiple isotope systems on small ({\\textless} 300 μm) melt inclusions was hampered by analytical limitations. Here we report the first coupled Sr-Nd-Pb isotope data on individual melt inclusions from potassium-rich lavas from neighbouring Quaternary volcanoes in central Italy and infer the presence of a previously unidentified ancient lower crustal component in the mantle. We suggest derivation from Variscan or older basement included in the upper mantle by either delamination, sediment recycling, subduction erosion and/or slab detachment processes during Cenozoic subduction and collision of the western Mediterranean. The capability to determine isotope ratios in individual melt inclusions permits the detection of distinctive mantle contaminants and can provide insights into how geodynamic processes affect subduction recycling.},\n\tlanguage = {en},\n\tnumber = {1},\n\turldate = {2021-09-08},\n\tjournal = {Nature Communications},\n\tauthor = {Koornneef, Janne M. and Nikogosian, Igor and van Bergen, Manfred J. and Vroon, Pieter Z. and Davies, Gareth R.},\n\tmonth = jul,\n\tyear = {2019},\n\tpages = {3237},\n}\n\n

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\n \n\n \n \n \n \n \n \n Ultra-small microorganisms in the polyextreme conditions of the Dallol volcano, Northern Afar, Ethiopia.\n \n \n \n \n\n\n \n Gómez, F.; Cavalazzi, B.; Rodríguez, N.; Amils, R.; Ori, G. G.; Olsson-Francis, K.; Escudero, C.; Martínez, J. M.; and Miruts, H.\n\n\n \n\n\n\n Scientific Reports, 9(1): 7907. May 2019.\n \n\n\n\n
\n\n\n\n \n \n $\"Ultra-small$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{gomez_ultra-small_2019,\n\ttitle = {Ultra-small microorganisms in the polyextreme conditions of the {Dallol} volcano, {Northern} {Afar}, {Ethiopia}},\n\tvolume = {9},\n\tcopyright = {2019 The Author(s)},\n\tissn = {2045-2322},\n\turl = {https://www.nature.com/articles/s41598-019-44440-8},\n\tdoi = {10.1038/s41598-019-44440-8},\n\tabstract = {The Dallol geothermal area in the northern part of the Danakil Depression (up to 124–155 meter below sea level) is deemed one of the most extreme environments on Earth. The area is notable for being part of the Afar Depression, an incipient seafloor-spreading center located at the triple junction, between Nubian, Somali and Arabian plates, and for hosting environments at the very edge of natural physical-chemical extremities. The northern part of the Danakil Depression is dominated by the Assale salt plain (an accumulation of marine evaporite deposits) and hosts the Dallol volcano. Here, the interaction between the evaporitic deposit and the volcanisms have created the unique Dallol hot springs, which are highly acidic (pH {\\textasciitilde} 0) and saline (saturation) with maximum temperatures ranging between 90 and 109 °C. Here we report for the first time evidence of life existing with these hot springs using a combination of morphological and molecular analyses. Ultra-small structures are shown to be entombed within mineral deposits, which are identified as members of the Order Nanohaloarchaea. The results from this study suggest the microorganisms can survive, and potential live, within this extreme environment, which has implications for understanding the limits of habitability on Earth and on (early) Mars.},\n\tlanguage = {en},\n\tnumber = {1},\n\turldate = {2021-09-08},\n\tjournal = {Scientific Reports},\n\tauthor = {Gómez, Felipe and Cavalazzi, Barbara and Rodríguez, Nuria and Amils, Ricardo and Ori, Gian Gabriele and Olsson-Francis, Karen and Escudero, Cristina and Martínez, Jose M. and Miruts, Hagos},\n\tmonth = may,\n\tyear = {2019},\n\tpages = {7907},\n}\n\n

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\n \n\n \n \n \n \n \n \n Some things special about NEAs: Geometric and environmental effects on the optical signatures of hydration.\n \n \n \n \n\n\n \n Potin, S.; Beck, P.; Schmitt, B.; and Moynier, F.\n\n\n \n\n\n\n Icarus, 333: 415–428. November 2019.\n \n\n\n\n
\n\n\n\n \n \n $\"Some$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{potin_things_2019,\n\ttitle = {Some things special about {NEAs}: {Geometric} and environmental effects on the optical signatures of hydration},\n\tvolume = {333},\n\tissn = {0019-1035},\n\tshorttitle = {Some things special about {NEAs}},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0019103519301162},\n\tdoi = {10.1016/j.icarus.2019.06.026},\n\tabstract = {Here were report on a laboratory study aiming to reproduce specificities of near-Earth Asteroid. We study how the elevated surface temperature, their surface roughness (rock or regolith), as well as observation geometry can affect the absorption features detected on asteroids. For that purpose, we selected a recent carbonaceous chondrite fall, the Mukundpura CM2 chondrite which fell in India in June 2017. Bidirectional reflectance spectroscopy was performed to analyze the effect of the geometrical configuration (incidence, emergence and azimuth angle) on the measurement. Our results show that reflectance spectra obtained under warm environment (NEA-like) tends to show shallower absorption bands compared to low-temperature conditions (MBA-like), but still detectable in our experiments under laboratory timescales. Irreversible alteration of the sample because of the warm environment (from room temperature to 250 °C) has been detected as an increase of the spectral slope and a decrease of the band depths (at 0.7 μm, 0.9 μm and 2.7 μm). Comparing the meteoritic chip and the powdered sample, we found that surface texture strongly affects the shape of the reflectance spectra of meteorites and thus of asteroids, where a dust-covered surface presents deeper absorption features. We found that all spectral parameters, such as the reflectance value, spectral slope and possible absorption bands are affected by the geometry of measurement. We observed the disappearance of the 0.7 μm absorption feature at phase angle larger than 120°, but the 3 μm band remains detectable on all measured spectra.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Icarus},\n\tauthor = {Potin, S. and Beck, P. and Schmitt, B. and Moynier, F.},\n\tmonth = nov,\n\tyear = {2019},\n\tpages = {415--428},\n}\n\n

\n\n\n\n\n\n

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\n \n\n \n \n \n \n \n \n Laboratory study of aerosol settling velocities using Laser Doppler velocimetry.\n \n \n \n \n\n\n \n Jakobsen, A. B.; Merrison, J.; and Iversen, J. J.\n\n\n \n\n\n\n Journal of Aerosol Science, 135: 58–71. September 2019.\n \n\n\n\n
\n\n\n\n \n \n $\"Laboratory$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{jakobsen_laboratory_2019,\n\ttitle = {Laboratory study of aerosol settling velocities using {Laser} {Doppler} velocimetry},\n\tvolume = {135},\n\tissn = {0021-8502},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0021850218301733},\n\tdoi = {10.1016/j.jaerosci.2019.05.003},\n\tabstract = {As a method to experimentally study aerodynamic drag the terminal settling velocities of aerosolized silica and glass microspheres (with sizes of 1–44 μm) have been measured at various gas pressures in the range 0.6–10 mbar and using various gas compositions including He, Ar, Xe, Air, CO2, and water vapour. Within the molecular scattering regime, i.e. where the Knudsen number Kn {\\textgreater} 10 and up to 500, reasonable agreement has been found with the model of Epstein (1924). Values of the scattering parameter δ were observed to be within the expected range of 1–1.44 for respectively specular/evaporative - diffuse molecular scattering processes. However, δ was seen to depend upon gas composition, specifically for H2O; δ = 0.96 ± 0.07, CO2; δ = 1.16 ± 0.07, noble gasses; δ = 1.25–1.44 and in the case of Air δ = 1.18 ± 0.07 which is not in agreement with that conventionally used of around 1.3–1.4. These observations imply disagreement with the concept of a general or universal model of drag for all particle surfaces and atmospheres. Similarly, for Kn {\\textless} 10 these results were not well described by conventional models such as the semi-empirical expression of Knudsen-Weber (1911) or the general law of fall proposed by Millikan (1923b).},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Journal of Aerosol Science},\n\tauthor = {Jakobsen, Andreas Boes and Merrison, Jonathan and Iversen, Jens Jacob},\n\tmonth = sep,\n\tyear = {2019},\n\tpages = {58--71},\n}\n\n

\n\n\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Spectral behavior of sulfides in simulated daytime surface conditions of Mercury: Supporting past (MESSENGER) and future missions (BepiColombo).\n \n \n \n \n\n\n \n Varatharajan, I.; Maturilli, A.; Helbert, J.; Alemanno, G.; and Hiesinger, H.\n\n\n \n\n\n\n Earth and Planetary Science Letters, 520: 127–140. August 2019.\n \n\n\n\n
\n\n\n\n \n \n $\"Spectral$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{varatharajan_spectral_2019,\n\ttitle = {Spectral behavior of sulfides in simulated daytime surface conditions of {Mercury}: {Supporting} past ({MESSENGER}) and future missions ({BepiColombo})},\n\tvolume = {520},\n\tissn = {0012-821X},\n\tshorttitle = {Spectral behavior of sulfides in simulated daytime surface conditions of {Mercury}},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0012821X19302900},\n\tdoi = {10.1016/j.epsl.2019.05.020},\n\tabstract = {To detect the mineral diversity of a planet's surface, it is essential to study the spectral variations over a broad wavelength range at relevant simulated laboratory conditions. The MESSENGER (Mercury Surface, Space Environment, Geochemistry, and Ranging) mission to Mercury discovered that irrespective of its formation closest to the Sun, Mercury is richer in volatiles than previously expected. This is especially true for sulfur (S), with an average abundance of 4 wt\\%. It has been proposed that sulfur in the interior of Mercury can be brought to the surface through volcanic activity in the form of sulfides as slag deposits in Mercury hollows and pyroclastic deposits. However, comprehensive spectral library of sulfide minerals measured under vacuum conditions in a wide spectral range (0.2–100 μm) was lacking. This affects the detectability and understanding of the distribution, abundance, and type of sulfides on Mercury using remote-sensing spectral observations. In the case of Mercury, the effect of thermal weathering affecting the spectral behavior of these sulfides must be studied carefully for their effective detection. In this study, we present a spectral library of synthetic sulfides including MgS, FeS, CaS, CrS, TiS, NaS, and MnS. For each sample, we performed emissivity measurements in the thermal infrared range (TIR: ∼7–14 μm) for sample temperatures from 100°C–500°C, covering the daytime temperature cycle on Mercury's surface. In addition, for each sample we measured the spectral reflectance of fresh and thermally processed sulfides over a wide spectral range (0.2–100 μm) and at four different phase angles, 26°, 40°, 60°, 80°. This spectral library facilitates the detection of sulfides by past and future missions to Mercury by any optical spectrometer of any spectral range. Specifically, the emissivity measurements in this study will support the Mercury Radiometer and Thermal Imaging Spectrometer (MERTIS) instrument on the ESA/JAXA BepiColombo mission, which will study the surface mineralogy over a wavelength range of 7–14 μm at a spatial resolution of 500 m/pixel. The measured reflectance of these sulfides in 0.2–100 μm at various phase angles will support the interpretation of measurements from past (MDIS, MASCS on MESSENGER) and future missions (SIMBIO-SYS on BepiColombo).},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Earth and Planetary Science Letters},\n\tauthor = {Varatharajan, I. and Maturilli, A. and Helbert, J. and Alemanno, G. and Hiesinger, H.},\n\tmonth = aug,\n\tyear = {2019},\n\tkeywords = {Mercury, emissivity, reflectance, spectroscopy, sulfides},\n\tpages = {127--140},\n}\n\n

\n\n\n

\n To detect the mineral diversity of a planet's surface, it is essential to study the spectral variations over a broad wavelength range at relevant simulated laboratory conditions. The MESSENGER (Mercury Surface, Space Environment, Geochemistry, and Ranging) mission to Mercury discovered that irrespective of its formation closest to the Sun, Mercury is richer in volatiles than previously expected. This is especially true for sulfur (S), with an average abundance of 4 wt%. It has been proposed that sulfur in the interior of Mercury can be brought to the surface through volcanic activity in the form of sulfides as slag deposits in Mercury hollows and pyroclastic deposits. However, comprehensive spectral library of sulfide minerals measured under vacuum conditions in a wide spectral range (0.2–100 μm) was lacking. This affects the detectability and understanding of the distribution, abundance, and type of sulfides on Mercury using remote-sensing spectral observations. In the case of Mercury, the effect of thermal weathering affecting the spectral behavior of these sulfides must be studied carefully for their effective detection. In this study, we present a spectral library of synthetic sulfides including MgS, FeS, CaS, CrS, TiS, NaS, and MnS. For each sample, we performed emissivity measurements in the thermal infrared range (TIR: ∼7–14 μm) for sample temperatures from 100°C–500°C, covering the daytime temperature cycle on Mercury's surface. In addition, for each sample we measured the spectral reflectance of fresh and thermally processed sulfides over a wide spectral range (0.2–100 μm) and at four different phase angles, 26°, 40°, 60°, 80°. This spectral library facilitates the detection of sulfides by past and future missions to Mercury by any optical spectrometer of any spectral range. Specifically, the emissivity measurements in this study will support the Mercury Radiometer and Thermal Imaging Spectrometer (MERTIS) instrument on the ESA/JAXA BepiColombo mission, which will study the surface mineralogy over a wavelength range of 7–14 μm at a spatial resolution of 500 m/pixel. The measured reflectance of these sulfides in 0.2–100 μm at various phase angles will support the interpretation of measurements from past (MDIS, MASCS on MESSENGER) and future missions (SIMBIO-SYS on BepiColombo).\n

\n\n\n

\n \n\n \n \n \n \n \n \n Geomicrobiology of a seawater-influenced active sulfuric acid cave.\n \n \n \n \n\n\n \n D’Angeli, I. M.; Ghezzi, D.; Leuko, S.; Firrincieli, A.; Parise, M.; Fiorucci, A.; Vigna, B.; Addesso, R.; Baldantoni, D.; Carbone, C.; Miller, A. Z.; Jurado, V.; Saiz-Jimenez, C.; Waele, J. D.; and Cappelletti, M.\n\n\n \n\n\n\n PLOS ONE, 14(8): e0220706. August 2019.\n \n\n\n\n
\n\n\n\n \n \n $\"Geomicrobiology$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{dangeli_geomicrobiology_2019,\n\ttitle = {Geomicrobiology of a seawater-influenced active sulfuric acid cave},\n\tvolume = {14},\n\tissn = {1932-6203},\n\turl = {https://journals.plos.org/plosone/article?id=10.1371/journal.pone.0220706},\n\tdoi = {10.1371/journal.pone.0220706},\n\tabstract = {Fetida Cave is an active sulfuric acid cave influenced by seawater, showing abundant microbial communities that organize themselves under three main different morphologies: water filaments, vermiculations and moonmilk deposits. These biofilms/deposits have different cave distribution, pH, macro- and microelement and mineralogical composition, carbon and nitrogen content. In particular, water filaments and vermiculations had circumneutral and slightly acidic pH, respectively, both had abundant organic carbon and high microbial diversity. They were rich in macro- and microelements, deriving from mineral dissolution, and, in the case of water filaments, from seawater composition. Vermiculations had different color, partly associated with their mineralogy, and unusual minerals probably due to trapping capacities. Moonmilk was composed of gypsum, poor in organic matter, had an extremely low pH (0–1) and low microbial diversity. Based on 16S rRNA gene analysis, the microbial composition of the biofilms/deposits included autotrophic taxa associated with sulfur and nitrogen cycles and biomineralization processes. In particular, water filaments communities were characterized by bacterial taxa involved in sulfur oxidation and reduction in aquatic, aphotic, microaerophilic/anoxic environments (Campylobacterales, Thiotrichales, Arenicellales, Desulfobacterales, Desulforomonadales) and in chemolithotrophy in marine habitats (Oceanospirillales, Chromatiales). Their biodiversity was linked to the morphology of the water filaments and their collection site. Microbial communities within vermiculations were partly related to their color and showed high abundance of unclassified Betaproteobacteria and sulfur-oxidizing Hydrogenophilales (including Sulfuriferula), and Acidiferrobacterales (including Sulfurifustis), sulfur-reducing Desulfurellales, and ammonia-oxidizing Planctomycetes and Nitrospirae. The microbial community associated with gypsum moonmilk showed the strong dominance ({\\textgreater}60\\%) of the archaeal genus Thermoplasma and lower abundance of chemolithotrophic Acidithiobacillus, metal-oxidizing Metallibacterium, Sulfobacillus, and Acidibacillus. This study describes the geomicrobiology of water filaments, vermiculations and gypsum moonmilk from Fetida Cave, providing insights into the microbial taxa that characterize each morphology and contribute to biogeochemical cycles and speleogenesis of this peculiar seawater-influenced sulfuric acid cave.},\n\tlanguage = {en},\n\tnumber = {8},\n\turldate = {2021-09-08},\n\tjournal = {PLOS ONE},\n\tauthor = {D’Angeli, Ilenia M. and Ghezzi, Daniele and Leuko, Stefan and Firrincieli, Andrea and Parise, Mario and Fiorucci, Adriano and Vigna, Bartolomeo and Addesso, Rosangela and Baldantoni, Daniela and Carbone, Cristina and Miller, Ana Zelia and Jurado, Valme and Saiz-Jimenez, Cesareo and Waele, Jo De and Cappelletti, Martina},\n\tmonth = aug,\n\tyear = {2019},\n\tkeywords = {Acid deposition, Bacterial biofilms, Biofilms, Caves, Geochemistry, Microbial ecosystems, Sea water, Sulfur},\n\tpages = {e0220706},\n}\n\n

\n\n\n

\n Fetida Cave is an active sulfuric acid cave influenced by seawater, showing abundant microbial communities that organize themselves under three main different morphologies: water filaments, vermiculations and moonmilk deposits. These biofilms/deposits have different cave distribution, pH, macro- and microelement and mineralogical composition, carbon and nitrogen content. In particular, water filaments and vermiculations had circumneutral and slightly acidic pH, respectively, both had abundant organic carbon and high microbial diversity. They were rich in macro- and microelements, deriving from mineral dissolution, and, in the case of water filaments, from seawater composition. Vermiculations had different color, partly associated with their mineralogy, and unusual minerals probably due to trapping capacities. Moonmilk was composed of gypsum, poor in organic matter, had an extremely low pH (0–1) and low microbial diversity. Based on 16S rRNA gene analysis, the microbial composition of the biofilms/deposits included autotrophic taxa associated with sulfur and nitrogen cycles and biomineralization processes. In particular, water filaments communities were characterized by bacterial taxa involved in sulfur oxidation and reduction in aquatic, aphotic, microaerophilic/anoxic environments (Campylobacterales, Thiotrichales, Arenicellales, Desulfobacterales, Desulforomonadales) and in chemolithotrophy in marine habitats (Oceanospirillales, Chromatiales). Their biodiversity was linked to the morphology of the water filaments and their collection site. Microbial communities within vermiculations were partly related to their color and showed high abundance of unclassified Betaproteobacteria and sulfur-oxidizing Hydrogenophilales (including Sulfuriferula), and Acidiferrobacterales (including Sulfurifustis), sulfur-reducing Desulfurellales, and ammonia-oxidizing Planctomycetes and Nitrospirae. The microbial community associated with gypsum moonmilk showed the strong dominance (\\textgreater60%) of the archaeal genus Thermoplasma and lower abundance of chemolithotrophic Acidithiobacillus, metal-oxidizing Metallibacterium, Sulfobacillus, and Acidibacillus. This study describes the geomicrobiology of water filaments, vermiculations and gypsum moonmilk from Fetida Cave, providing insights into the microbial taxa that characterize each morphology and contribute to biogeochemical cycles and speleogenesis of this peculiar seawater-influenced sulfuric acid cave.\n

\n\n\n

\n \n\n \n \n \n \n \n \n Titanium isotopic evidence for a shared genetic heritage of refractory inclusions from different carbonaceous chondrites.\n \n \n \n \n\n\n \n Render, J.; Ebert, S.; Burkhardt, C.; Kleine, T.; and Brennecka, G. A.\n\n\n \n\n\n\n Geochimica et Cosmochimica Acta, 254: 40–53. June 2019.\n \n\n\n\n
\n\n\n\n \n \n $\"Titanium$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{render_titanium_2019,\n\ttitle = {Titanium isotopic evidence for a shared genetic heritage of refractory inclusions from different carbonaceous chondrites},\n\tvolume = {254},\n\tissn = {0016-7037},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0016703719301498},\n\tdoi = {10.1016/j.gca.2019.03.011},\n\tabstract = {Insights into the earliest stages of our Solar System can be derived from its oldest dated solids, calcium-aluminum-rich inclusions (CAIs). In particular, investigating isotopic anomalies of nucleosynthetic origin in CAIs offers potential clues to the genetic heritage of refractory inclusions and the reservoir(s) involved in their formation. To this point, however, nucleosynthetic anomalies in refractory inclusions have almost exclusively been recognized in (1) relatively large CAIs from CV3 chondrites, employing chemical purification and high-precision mass spectrometry, or (2) from sub-mm-sized hibonite-rich objects (e.g., PLACs, SHIBs) from the Murchison CM2 chondrite using much less precise in-situ techniques. Whereas the latter have been shown to be highly anomalous in their isotopic compositions, their genetic connection to ‘regular’ CAIs from carbonaceous chondrites remains poorly understood. Here, we aim to address this issue by taking advantage of a new technique that allows for high-precision analysis of sub-mm-sized inclusions. Using this method, we report Ti isotope anomalies in a suite of twelve CAIs from five different CO carbonaceous chondrites, as well as ten refractory inclusions from the CM2 chondrite Jbilet Winselwan using MC-ICPMS. We find that these CO and CM CAIs exhibit Ti isotopic compositions very similar to those of previously investigated CV3 (and of two CK3) CAIs, suggesting a fundamental genetic relationship of CAIs found within these chondrite groups. As such, our data indicates that CAIs from various groups of carbonaceous chondrites formed from similar matter and in a single region of the solar nebula (i.e., derived from a single common CAI-formation region). Collectively, these data show evidence of large-scale transport of CAIs over a significant range of heliocentric distances, covering at least the accretion areas of the CV, CK, CO, and CM chondrites. In addition, we report two inclusions consisting of hibonite-rich crystal aggregates from Jbilet Winselwan that exhibit highly irregular nucleosynthetic Ti signatures, implying a distinct origin from the aforementioned CAIs. These inclusions may represent an earlier generation of refractory material, perhaps more akin to the previously mentioned PLACs and/or SHIBs.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Geochimica et Cosmochimica Acta},\n\tauthor = {Render, Jan and Ebert, Samuel and Burkhardt, Christoph and Kleine, Thorsten and Brennecka, Gregory A.},\n\tmonth = jun,\n\tyear = {2019},\n\tkeywords = {CM chondrites, CO chondrites, Early solar system, Nucleosynthetic isotopic anomalies, Refractory inclusions, Titanium},\n\tpages = {40--53},\n}\n\n

\n\n\n

\n Insights into the earliest stages of our Solar System can be derived from its oldest dated solids, calcium-aluminum-rich inclusions (CAIs). In particular, investigating isotopic anomalies of nucleosynthetic origin in CAIs offers potential clues to the genetic heritage of refractory inclusions and the reservoir(s) involved in their formation. To this point, however, nucleosynthetic anomalies in refractory inclusions have almost exclusively been recognized in (1) relatively large CAIs from CV3 chondrites, employing chemical purification and high-precision mass spectrometry, or (2) from sub-mm-sized hibonite-rich objects (e.g., PLACs, SHIBs) from the Murchison CM2 chondrite using much less precise in-situ techniques. Whereas the latter have been shown to be highly anomalous in their isotopic compositions, their genetic connection to ‘regular’ CAIs from carbonaceous chondrites remains poorly understood. Here, we aim to address this issue by taking advantage of a new technique that allows for high-precision analysis of sub-mm-sized inclusions. Using this method, we report Ti isotope anomalies in a suite of twelve CAIs from five different CO carbonaceous chondrites, as well as ten refractory inclusions from the CM2 chondrite Jbilet Winselwan using MC-ICPMS. We find that these CO and CM CAIs exhibit Ti isotopic compositions very similar to those of previously investigated CV3 (and of two CK3) CAIs, suggesting a fundamental genetic relationship of CAIs found within these chondrite groups. As such, our data indicates that CAIs from various groups of carbonaceous chondrites formed from similar matter and in a single region of the solar nebula (i.e., derived from a single common CAI-formation region). Collectively, these data show evidence of large-scale transport of CAIs over a significant range of heliocentric distances, covering at least the accretion areas of the CV, CK, CO, and CM chondrites. In addition, we report two inclusions consisting of hibonite-rich crystal aggregates from Jbilet Winselwan that exhibit highly irregular nucleosynthetic Ti signatures, implying a distinct origin from the aforementioned CAIs. These inclusions may represent an earlier generation of refractory material, perhaps more akin to the previously mentioned PLACs and/or SHIBs.\n

\n\n\n

\n \n\n \n \n \n \n \n \n The newly improved set-up at the Planetary Spectroscopy Laboratory (PSL).\n \n \n \n \n\n\n \n Maturilli, A.; Helbert, J.; and Arnold, G.\n\n\n \n\n\n\n , 11128: 111280T. September 2019.\n ADS Bibcode: 2019SPIE11128E..0TM\n\n\n\n
\n\n\n\n \n \n $\"The$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{2019SPIE11128E..0TM,\n\ttitle = {The newly improved set-up at the {Planetary} {Spectroscopy} {Laboratory} ({PSL})},\n\tvolume = {11128},\n\turl = {https://ui.adsabs.harvard.edu/abs/2019SPIE11128E..0TM},\n\tdoi = {10.1117/12.2529266},\n\tabstract = {The Planetary Spectroscopy Laboratory (PSL) of DLR in Berlin provides spectral measurements of primarily planetary analogues from the visible to the far-infrared range. PSL has supported the data analysis as well as the development and calibration of instruments for planetary missions from ESA, NASA and JAXA. For this purposes PSL provides reflection, transmission and emission spectroscopy of target materials. Currently PSL operates three identical Bruker Vertex 80V vacuum FTIR spectrometer (the third one just installed in June 2019), two spectrometers are equipped with aluminum mirrors optimized for the UV, visible and near-IR, the third features gold-coated mirrors for the near to far IR spectral range. External simulation chambers are attached to two of the instruments for emissivity measurements. The chamber at the near to far IR instrument allows emissivity measurements from 0.7-200 μm under vacuum for sample temperatures from 320K to above 900K, using an innovative induction system. The second chamber (purged with dry air and water cooled to {\\textless}=270K) allows emissivity measurements of samples with surface temperature from 290K to 420K. We measure bi-directional reflectance of samples; with variable incidence and emission angles between 0° and 85° (minimum phase angle is 26° to prevent damages to the mirrors). Samples are measured currently at room temperature and 170K, with a planned extension for temperatures below 100K, by means of a new external chamber, whose funding is accepted and will be available in 2020. Bi-directional and hemispherical reflectance is measured under purging/vacuum conditions, covering the 0.2 to above 200 μm spectral range. An FT-IR microscope installed at the end of 2018, allows microscopic analysis in transmission and reflectance in the VIS+VNIR+MIR spectral range. Transmission of thin slabs, optical filters, optical windows, pellets, and others is measured in the complete spectral range from UV to FIR using a parallel beam configuration to avoid refraction},\n\turldate = {2021-09-08},\n\tauthor = {Maturilli, A. and Helbert, J. and Arnold, G.},\n\tmonth = sep,\n\tyear = {2019},\n\tnote = {ADS Bibcode: 2019SPIE11128E..0TM},\n\tpages = {111280T},\n}\n\n

\n\n\n

\n The Planetary Spectroscopy Laboratory (PSL) of DLR in Berlin provides spectral measurements of primarily planetary analogues from the visible to the far-infrared range. PSL has supported the data analysis as well as the development and calibration of instruments for planetary missions from ESA, NASA and JAXA. For this purposes PSL provides reflection, transmission and emission spectroscopy of target materials. Currently PSL operates three identical Bruker Vertex 80V vacuum FTIR spectrometer (the third one just installed in June 2019), two spectrometers are equipped with aluminum mirrors optimized for the UV, visible and near-IR, the third features gold-coated mirrors for the near to far IR spectral range. External simulation chambers are attached to two of the instruments for emissivity measurements. The chamber at the near to far IR instrument allows emissivity measurements from 0.7-200 μm under vacuum for sample temperatures from 320K to above 900K, using an innovative induction system. The second chamber (purged with dry air and water cooled to \\textless=270K) allows emissivity measurements of samples with surface temperature from 290K to 420K. We measure bi-directional reflectance of samples; with variable incidence and emission angles between 0° and 85° (minimum phase angle is 26° to prevent damages to the mirrors). Samples are measured currently at room temperature and 170K, with a planned extension for temperatures below 100K, by means of a new external chamber, whose funding is accepted and will be available in 2020. Bi-directional and hemispherical reflectance is measured under purging/vacuum conditions, covering the 0.2 to above 200 μm spectral range. An FT-IR microscope installed at the end of 2018, allows microscopic analysis in transmission and reflectance in the VIS+VNIR+MIR spectral range. Transmission of thin slabs, optical filters, optical windows, pellets, and others is measured in the complete spectral range from UV to FIR using a parallel beam configuration to avoid refraction\n

\n\n\n

\n \n\n \n \n \n \n \n \n Characterization and first results of the planetary borehole-wall imager — methods to develop for in-situ exploration.\n \n \n \n \n\n\n \n Kereszturi, Á.; Duvet, L.; Gróf, G.; Gyenis, Á.; Gyenis, T.; Kapui, Z.; Kovács, B.; and Maros, G.\n\n\n \n\n\n\n Open Astronomy, 28(1): 13–31. January 2019.\n \n\n\n\n
\n\n\n\n \n \n $\"Characterization$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{kereszturi_characterization_2019,\n\ttitle = {Characterization and first results of the planetary borehole-wall imager — methods to develop for in-situ exploration},\n\tvolume = {28},\n\tissn = {2543-6376},\n\turl = {https://www.degruyter.com/document/doi/10.1515/astro-2019-0001/html},\n\tdoi = {10.1515/astro-2019-0001},\n\tabstract = {Prototypes of borehole-wall imager instruments were developed and tested at a desert riverbed in Morocco and at a lake’s salty flat in the Atacama desert, to support the drilling activity of ExoMars rover. The onsite recorded borehole images contain information on the context that are lost during the sample acquisition. Benefits of the borehole-wall imaging is the easier maximal energy estimation of a fluvial flow, the detailed information on sedimentation and layering, especially the former existence of liquid water and its temporal changes, including paleo-flow direction estimation from grain imbrication direction. Benefits of laboratory analysis of the acquired samples are the better identification of mineral types, determination of the level of maturity of granular sediment, and identification of the smallest, wet weathered grains. Based on the lessons learned during the comparison of field and laboratory results, we demonstrate that recording the borehole-wall with optical instrument during/after drilling on Mars supports the paleo-environment reconstruction with such data that would otherwise be lost during the sample acquisition. Because of the lack of plate tectonism and the low geothermal gradient on Mars, even Ga old sediments provide observable features that are especially important for targeting Mars sample return and later crewed Mars missions.},\n\tlanguage = {en},\n\tnumber = {1},\n\turldate = {2021-09-08},\n\tjournal = {Open Astronomy},\n\tauthor = {Kereszturi, Ákos and Duvet, Ludovic and Gróf, Gyula and Gyenis, Ákos and Gyenis, Tamás and Kapui, Zsuzsanna and Kovács, Bálint and Maros, Gyula},\n\tmonth = jan,\n\tyear = {2019},\n\tpages = {13--31},\n}\n\n

\n\n\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Laser-induced breakdown spectroscopy acoustic testing of the Mars 2020 microphone.\n \n \n \n \n\n\n \n Murdoch, N.; Chide, B.; Lasue, J.; Cadu, A.; Sournac, A.; Bassas-Portús, M.; Jacob, X.; Merrison, J.; Iversen, J. J.; Moretto, C.; Velasco, C.; Parès, L.; Hynes, A.; Godiver, V.; Lorenz, R. D.; Cais, P.; Bernadi, P.; Maurice, S.; Wiens, R. C.; and Mimoun, D.\n\n\n \n\n\n\n Planetary and Space Science, 165: 260–271. January 2019.\n \n\n\n\n
\n\n\n\n \n \n $\"Laser-induced$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{murdoch_laser-induced_2019,\n\ttitle = {Laser-induced breakdown spectroscopy acoustic testing of the {Mars} 2020 microphone},\n\tvolume = {165},\n\tissn = {0032-0633},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0032063318301375},\n\tdoi = {10.1016/j.pss.2018.09.009},\n\tabstract = {The SuperCam instrument suite onboard the Mars 2020 rover will include the Mars Microphone, an experiment designed to record the sounds of the SuperCam laser strikes on rocks and also aeolian noise. In order to record shock waves produced by the laser blasts, the Mars Microphone must be able to record audio signals from 100 Hz to 10 kHz on the surface of Mars, with a sensitivity sufficient to monitor a laser impact at distances up to 4 m. The Aarhus planetary simulator facility has been used to test the Mars 2020 rover microphone in a controlled Martian environment. The end-to-end tests performed in a 6 mbar CO2 atmosphere, with wind, and also with the microphone at −80° C have demonstrated that the SuperCam/Mars Microphone requirements are satisfied. Tests were also performed on Martian soil simulant targets showing that the variation of the acoustic energy of the shock wave depends on the level of compaction of the target.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Planetary and Space Science},\n\tauthor = {Murdoch, N. and Chide, B. and Lasue, J. and Cadu, A. and Sournac, A. and Bassas-Portús, M. and Jacob, X. and Merrison, J. and Iversen, J. J. and Moretto, C. and Velasco, C. and Parès, L. and Hynes, A. and Godiver, V. and Lorenz, R. D. and Cais, P. and Bernadi, P. and Maurice, S. and Wiens, R. C. and Mimoun, D.},\n\tmonth = jan,\n\tyear = {2019},\n\tkeywords = {Atmosphere, Laser-induced breakdown spectroscopy, Mars 2020, Mars microphone, Soil compaction, SuperCam},\n\tpages = {260--271},\n}\n\n

\n\n\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n The Dependence of Spectral Features on Ice Content and Temperature for Vesta and Ryugu.\n \n \n \n\n\n \n Michalik, T.; Maturilli, A.; Otto, K.; Schmitt, B.; Poch, O.; Beck, P.; and Helbert, J.\n\n\n \n\n\n\n In volume 2132, The Woodlands, Texas, March 2019. LPI Contribution\n id.1984\n\n\n\n
\n\n\n\n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@inproceedings{michalik_dependence_2019,\n\taddress = {The Woodlands, Texas},\n\ttitle = {The {Dependence} of {Spectral} {Features} on {Ice} {Content} and {Temperature} for {Vesta} and {Ryugu}},\n\tvolume = {2132},\n\tlanguage = {en},\n\tpublisher = {LPI Contribution},\n\tauthor = {Michalik, T. and Maturilli, A. and Otto, K. and Schmitt, B. and Poch, O. and Beck, P. and Helbert, J.},\n\tmonth = mar,\n\tyear = {2019},\n\tnote = {id.1984},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Laboratory analysis of Martian analogues for comparison with CRISM observations for detection of polycyclic aromatic hydrocarbons.\n \n \n \n \n\n\n \n Campbell, J.; Schmitt, B.; Brissaud, O.; and Muller, J.\n\n\n \n\n\n\n , 13: EPSC–DPS2019–1577. September 2019.\n \n\n\n\n
\n\n\n\n \n \n $\"Laboratory$ Paper\n \n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{campbell_laboratory_2019,\n\ttitle = {Laboratory analysis of {Martian} analogues for comparison with {CRISM} observations for detection of polycyclic aromatic hydrocarbons},\n\tvolume = {13},\n\turl = {http://adsabs.harvard.edu/abs/2019EPSC...13.1577C},\n\tabstract = {The detection of organics on Mars is important to the quest for life \nbeyond Earth. This work uses laboratory experiments to simulate the\ncondition of dynamic features on Mars in order to compare to orbital\nobservations. The detectability limit of polycyclic aromatic\nhydrocarbons was established within Mars analogues for the South Polar\nResidual Cap and Recurring Slope Lineae, end member spectra have been\nestablished for all components of interest, and new diagnostic\nabsorption features for PAHs have been recorded at a number of\nwavelengths. For RSL analogues, we found that drying brines within soil\nsample increased the detectability of PAHs compared with soil samples\nvoid of salt.},\n\turldate = {2021-06-21},\n\tauthor = {Campbell, Jacqueline and Schmitt, Bernard and Brissaud, Olivier and Muller, Jan-Peter},\n\tmonth = sep,\n\tyear = {2019},\n\tpages = {EPSC--DPS2019--1577},\n}\n\n

\n\n\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n VIS-IR spectroscopy of mixtures of ice, organic matter and opaque mineral in support of minor bodies remote sensing observations.\n \n \n \n \n\n\n \n Ciarniello, M.; Moroz, L. V.; Poch, O.; Vinogradoff, V.; Beck, P.; Rousseau, B.; Istiqomah, I.; Sultana, R.; Raponi, A.; Schroeder, S.; Kappel, D.; Quirico, E.; Filacchione, G.; Pommerol, A.; Mennella, V.; and Pilorget, C.\n\n\n \n\n\n\n , 2019: EPSC–DPS2019–1467. September 2019.\n \n\n\n\n
\n\n\n\n \n \n $\"VIS-IR$ Paper\n \n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{ciarniello_vis-ir_2019,\n\ttitle = {{VIS}-{IR} spectroscopy of mixtures of ice, organic matter and opaque mineral in support of minor bodies remote sensing observations},\n\tvolume = {2019},\n\turl = {https://ui.adsabs.harvard.edu/abs/2019EPSC...13.1467C},\n\tabstract = {We investigate the VIS-IR spectral reflectance of mixtures rich in water ice and organics, in support of the interpretation of remote sensing observations of minor bodies from space missions, and to test the ability of radiative transfer models to infer surface composition from VIS-IR spectroscopy},\n\turldate = {2021-07-26},\n\tauthor = {Ciarniello, Mauro and Moroz, Ljuba V. and Poch, Olivier and Vinogradoff, Vassilissa and Beck, Pierre and Rousseau, Batiste and Istiqomah, Istiqomah and Sultana, Robin and Raponi, Andrea and Schroeder, Stefanus and Kappel, David and Quirico, Eric and Filacchione, Gianrico and Pommerol, Antoine and Mennella, Vito and Pilorget, Cedric},\n\tmonth = sep,\n\tyear = {2019},\n\tpages = {EPSC--DPS2019--1467},\n}\n\n

\n\n\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Spectral properties of H2O ice depending on particle size and surface temperature - comparison between laboratory data and icy satellites observations.\n \n \n \n \n\n\n \n Stephan, K.; Ciarniello, M.; Dalle Ore, C.; Cruikshank, D. P.; Filacchione, G.; Haack, D.; Jaumann, R.; Poch, O.; Raponi, A.; and Istigomah, I.\n\n\n \n\n\n\n , 2019: EPSC–DPS2019–1493. September 2019.\n \n\n\n\n
\n\n\n\n \n \n $\"Spectral$ Paper\n \n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{stephan_spectral_2019,\n\ttitle = {Spectral properties of {H2O} ice depending on particle size and surface temperature - comparison between laboratory data and icy satellites observations},\n\tvolume = {2019},\n\turl = {https://ui.adsabs.harvard.edu/abs/2019EPSC...13.1493S},\n\tabstract = {In order to support the investigation of the icy surface properties, we measured the spectral properties of H2O ice samples for temperatures between 70 and 150 K and analyzed the differences in the H2O ice spectral signature with particles size and temperature in comparison to the spectral properties of fresh impact craters in the Jovian and Saturnian systems.},\n\turldate = {2021-07-26},\n\tauthor = {Stephan, Katrin and Ciarniello, Mauro and Dalle Ore, Cristina and Cruikshank, Dale P. and Filacchione, Gianrico and Haack, David and Jaumann, Ralf and Poch, Oliver and Raponi, Andrea and Istigomah, Istigomah},\n\tmonth = sep,\n\tyear = {2019},\n\tpages = {EPSC--DPS2019--1493},\n}\n\n

\n\n\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Experimental evidence for the nature of Ceres blue material.\n \n \n \n \n\n\n \n Schröder, S.; Poch, O.; Ferrari, M.; De Angelis, S.; Sultana, R.; Potin, S.; Beck, P.; De Sanctis, M. C.; and Schmitt, B.\n\n\n \n\n\n\n , 2019: EPSC–DPS2019–78. September 2019.\n \n\n\n\n
\n\n\n\n \n \n $\"Experimental$ Paper\n \n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{schroder_experimental_2019,\n\ttitle = {Experimental evidence for the nature of {Ceres} blue material},\n\tvolume = {2019},\n\turl = {https://ui.adsabs.harvard.edu/abs/2019EPSC...13...78S},\n\tabstract = {The ejecta of young impact craters on Ceres are "blue", exhibiting a negative spectral slope in the visible and near-IR wavelength range, for reasons yet unknown. We have performed an experiment with Ceres analogue material to support the hypothesis that the blue color naturally results from the dehydration of phyllosilicate-rich ice particles, which are expected to form upon impact.},\n\turldate = {2021-07-26},\n\tauthor = {Schröder, Stefan and Poch, Olivier and Ferrari, Marco and De Angelis, Simone and Sultana, Robin and Potin, Sandra and Beck, Pierre and De Sanctis, Maria Cristina and Schmitt, Bernard},\n\tmonth = sep,\n\tyear = {2019},\n\tpages = {EPSC--DPS2019--78},\n}\n

\n\n\n\n\n\n

\n\n

\n \n 2018\n \n \n (15)\n \n \n

\n \n \n

\n \n\n \n \n \n \n \n \n Analysis of the products of a negative corona discharge in a N2–CH4 mixture with added CO2 used as a laboratory mimic of a prebiotic atmosphere.\n \n \n \n \n\n\n \n Mazankova, V.; Torokova, L.; Moravsky, L.; Matejcik, S.; Trunec, D.; Navratil, Z.; and Mason, N. J.\n\n\n \n\n\n\n Contributions to Plasma Physics, 58(10): 995–1004. 2018.\n \n\n\n\n
\n\n\n\n \n \n $\"Analysis$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n\n\n\n

@article{mazankova_analysis_2018,\n\ttitle = {Analysis of the products of a negative corona discharge in a {N2}–{CH4} mixture with added {CO2} used as a laboratory mimic of a prebiotic atmosphere},\n\tvolume = {58},\n\tissn = {1521-3986},\n\turl = {https://onlinelibrary.wiley.com/doi/abs/10.1002/ctpp.201700089},\n\tdoi = {10.1002/ctpp.201700089},\n\tabstract = {A negative corona discharge operating at atmospheric pressure has been used to initiate chemical reactions in a gaseous mixture of nitrogen, methane, and carbon dioxide. Such a mixture simulates the composition of the early Earth's atmosphere. This work extends our previous experimental studies of the chemistry of prebiotic atmospheres generated in an atmospheric-pressure glow discharge. The present work is devoted to the study of the role of CO2 in prebiotic atmospheric chemistry. The gas mixture was composed of nitrogen with 2–4\\% methane and 1\\% CO2. The corona discharge was characterized by electrical measurements and optical emission spectroscopy. The reaction products from the discharge were further analysed by Fourier transform infrared (FTIR) spectroscopy. The composition of solid products deposited on the electrode tip was obtained by energy dispersive X-ray (EDX) analysis. The specific input energy was altered during the experiments, and the concentration of all products was found to increase with its increase. It is further shown that while the addition of the CO2 admixture leads to the generation of CO and H2O, no other compounds containing oxygen were detected. The energy yields of products were calculated, and good agreement was found with the values obtained in previous experiments.},\n\tlanguage = {en},\n\tnumber = {10},\n\turldate = {2021-09-08},\n\tjournal = {Contributions to Plasma Physics},\n\tauthor = {Mazankova, V. and Torokova, L. and Moravsky, L. and Matejcik, S. and Trunec, D. and Navratil, Z. and Mason, N. J.},\n\tyear = {2018},\n\tkeywords = {FTIR spectroscopy, negative corona discharge, prebiotic atmosphere},\n\tpages = {995--1004},\n}\n\n

\n\n\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n What is controlling the reflectance spectra (0.35–150 µm) of hydrated (and dehydrated) carbonaceous chondrites?.\n \n \n \n \n\n\n \n Beck, P.; Maturilli, A.; Garenne, A.; Vernazza, P.; Helbert, J.; Quirico, E.; and Schmitt, B.\n\n\n \n\n\n\n Icarus, 313: 124–138. October 2018.\n \n\n\n\n
\n\n\n\n \n \n $\"What$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{beck_what_2018,\n\ttitle = {What is controlling the reflectance spectra (0.35–150 µm) of hydrated (and dehydrated) carbonaceous chondrites?},\n\tvolume = {313},\n\tissn = {0019-1035},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0019103517307807},\n\tdoi = {10.1016/j.icarus.2018.05.010},\n\tabstract = {In order to determine the controls on the reflectance spectra of hydrated carbonaceous chondrites, reflectance spectra were measured for a series of samples with well-determined mineralogy, water-content, and thermal history. This includes 5 CR chondrites, 11 CM chondrites, and 7 thermally metamorphosed CM chondrites. These samples were characterized over the 0.35–150 µm range by reflectance spectroscopy in order to cover the full spectral range accessible from ground based observation, and that will be determined in the near-future by the Hayabusa-2 and Osiris-REx missions. While spectra show absorption features shortward of 35 µm, no strong absorption bands were identified in this suite of samples longward of 35 µm. This work shows that the 0.7-µm band observed in hydrated carbonaceous chondrites is correlated with the total water content as well as with the band depth at 2.7 µm, confirming the suggestion that they are related to Mg-rich, Fe-bearing phyllosilicates. A feature at 2.3 µm, diagnostic of such phyllosilicates was found for all samples with a detectable 0.7-µm band, also indicative of Mg-rich phyllosilicates. A strong variability is found in the shape of the 3-µm band among CM chondrites, and between CM, CR and thermally metamorphosed CM chondrites. Heavily altered CM chondrites show a single strong band around 2.72 µm while more thermally metamorphosed CM samples show an absorption band at higher wavelength. The CR chondrite GRO 95577 has a 3-µm feature very similar to those of extensively altered CM chondrites while other CR chondrite rather shows goethite-like signatures (possibly due to terrestrial weathering of metals). Thermally metamorphosed CM chondrites all have 3-µm features, which are not purely due to terrestrial adsorbed water. The band shape ranges from heavily altered CM-like to goethite-like. The overall reflectance was found to be significantly higher for CR chondrites than for CM chondrites. This is also true for the hydrated CR chondrite GRO 95577 whose reflectance spectrum is almost identical to spectra obtained for CM chondrites except that it is brighter by about 40\\% in the visible. Another possibility to distinguish hydrated CM from hydrated CR chondrites is to use the combination of band depths at 0.7 and 2.3 µm. When comparing the spectra obtained with Cg and Cgh spectral end member, it is found that the band depth determined for hydrated chondrites (0.7 and 2.3 µm) are always higher than calculated for these spectral endmembers. If one considers only asteroids with unambiguous hydration detection, band depth at 0.7 µm is of similar value to those measured for hydrated carbonaceous chondrites.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Icarus},\n\tauthor = {Beck, Pierre and Maturilli, A. and Garenne, A. and Vernazza, P. and Helbert, J. and Quirico, E. and Schmitt, B.},\n\tmonth = oct,\n\tyear = {2018},\n\tkeywords = {Aqueous alteration, Asteroid, C-type, Infrared spectroscopy, Meteorites},\n\tpages = {124--138},\n}\n\n

\n\n\n

\n In order to determine the controls on the reflectance spectra of hydrated carbonaceous chondrites, reflectance spectra were measured for a series of samples with well-determined mineralogy, water-content, and thermal history. This includes 5 CR chondrites, 11 CM chondrites, and 7 thermally metamorphosed CM chondrites. These samples were characterized over the 0.35–150 µm range by reflectance spectroscopy in order to cover the full spectral range accessible from ground based observation, and that will be determined in the near-future by the Hayabusa-2 and Osiris-REx missions. While spectra show absorption features shortward of 35 µm, no strong absorption bands were identified in this suite of samples longward of 35 µm. This work shows that the 0.7-µm band observed in hydrated carbonaceous chondrites is correlated with the total water content as well as with the band depth at 2.7 µm, confirming the suggestion that they are related to Mg-rich, Fe-bearing phyllosilicates. A feature at 2.3 µm, diagnostic of such phyllosilicates was found for all samples with a detectable 0.7-µm band, also indicative of Mg-rich phyllosilicates. A strong variability is found in the shape of the 3-µm band among CM chondrites, and between CM, CR and thermally metamorphosed CM chondrites. Heavily altered CM chondrites show a single strong band around 2.72 µm while more thermally metamorphosed CM samples show an absorption band at higher wavelength. The CR chondrite GRO 95577 has a 3-µm feature very similar to those of extensively altered CM chondrites while other CR chondrite rather shows goethite-like signatures (possibly due to terrestrial weathering of metals). Thermally metamorphosed CM chondrites all have 3-µm features, which are not purely due to terrestrial adsorbed water. The band shape ranges from heavily altered CM-like to goethite-like. The overall reflectance was found to be significantly higher for CR chondrites than for CM chondrites. This is also true for the hydrated CR chondrite GRO 95577 whose reflectance spectrum is almost identical to spectra obtained for CM chondrites except that it is brighter by about 40% in the visible. Another possibility to distinguish hydrated CM from hydrated CR chondrites is to use the combination of band depths at 0.7 and 2.3 µm. When comparing the spectra obtained with Cg and Cgh spectral end member, it is found that the band depth determined for hydrated chondrites (0.7 and 2.3 µm) are always higher than calculated for these spectral endmembers. If one considers only asteroids with unambiguous hydration detection, band depth at 0.7 µm is of similar value to those measured for hydrated carbonaceous chondrites.\n

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\n \n\n \n \n \n \n \n \n Sr and Nd isotopic compositions of individual olivine-hosted melt inclusions from Hawai'i and Samoa: Implications for the origin of isotopic heterogeneity in melt inclusions from OIB lavas.\n \n \n \n \n\n\n \n Reinhard, A. A.; Jackson, M. G.; Koornneef, J. M.; Rose-Koga, E. F.; Blusztajn, J.; Konter, J. G.; Koga, K. T.; Wallace, P. J.; and Harvey, J.\n\n\n \n\n\n\n Chemical Geology, 495: 36–49. September 2018.\n \n\n\n\n
\n\n\n\n \n \n $\"Sr$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{reinhard_sr_2018,\n\ttitle = {Sr and {Nd} isotopic compositions of individual olivine-hosted melt inclusions from {Hawai}'i and {Samoa}: {Implications} for the origin of isotopic heterogeneity in melt inclusions from {OIB} lavas},\n\tvolume = {495},\n\tissn = {0009-2541},\n\tshorttitle = {Sr and {Nd} isotopic compositions of individual olivine-hosted melt inclusions from {Hawai}'i and {Samoa}},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0009254118303759},\n\tdoi = {10.1016/j.chemgeo.2018.07.034},\n\tabstract = {Geochemical investigations of mantle heterogeneity as sampled by ocean island basalts (OIB) have long relied on isotopic analyses of whole rock lavas. However recent work has shown that significant isotopic disequilibrium can exist between the phases (groundmass and phenocrysts) of a single OIB lava. In this study, we target individual olivine-hosted melt inclusions from two samples—one Samoan and one Hawai'ian—with melt inclusion 87Sr/86Sr heterogeneity previously measured using laser ablation inductively coupled plasma mass spectrometry (LA-ICP-MS). We report 87Sr/86Sr and 143Nd/144Nd in individual melt inclusions analyzed by thermal ionization mass spectrometry (TIMS). In melt inclusions from Samoan sample AVON3-71-2, we find highly heterogeneous (935 ppm) 87Sr/86Sr (0.705193–0.705853, N = 6), consistent with previously identified 87Sr/86Sr heterogeneity ({\\textasciitilde}2030 ppm) by laser ablation multi-collector ICP-MS (0.70459–0.70602, N = 12). In contrast, we find comparatively little (251 ppm) 87Sr/86Sr heterogeneity (0.703761–0.703938, N = 9) in olivine-hosted melt inclusions contained in a Hawaiian scoria clast from the Pu'u Wahi eruption (Mauna Loa). This result contrasts with a previous measurements by single-collector LA-ICP-MS that found highly heterogeneous ({\\textasciitilde}8500 ppm) 87Sr/86Sr in olivine-hosted melt inclusions from the same eruption (0.7021–0.7081, N = 137). In both the AVON3-71-2 and Pu'u Wahi melt inclusions, 143Nd/144Nd is indistinguishable from their respective whole rock 143Nd/144Nd values. The isotopic measurements on the melt inclusions are paired with major and trace element concentrations to investigate the mechanisms generating 87Sr/86Sr variability in melt inclusions. The lack of significant 87Sr/86Sr variability in the Hawai'ian melt inclusions (only 251 ppm) from Pu'u Wahi suggests a relatively simple magmatic history. In contrast, for the Samoan melt inclusions, we present evidence that supports the mixing of isotopically-heterogeneous mantle-derived melts as the mechanism generating the observed 87Sr/86Sr and trace element variability in the melt inclusions from AVON3-71-2. However, brine interaction appears to have increased the Cl concentrations of some of the Samoan inclusions without significantly modifying the 87Sr/86Sr or the other elemental budgets examined in this study.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Chemical Geology},\n\tauthor = {Reinhard, A. A. and Jackson, M. G. and Koornneef, J. M. and Rose-Koga, E. F. and Blusztajn, J. and Konter, J. G. and Koga, K. T. and Wallace, P. J. and Harvey, J.},\n\tmonth = sep,\n\tyear = {2018},\n\tkeywords = {Mantle geochemistry, Melt inclusions, Nd/Nd, Sr/Sr, TIMS},\n\tpages = {36--49},\n}\n\n

\n\n\n

\n Geochemical investigations of mantle heterogeneity as sampled by ocean island basalts (OIB) have long relied on isotopic analyses of whole rock lavas. However recent work has shown that significant isotopic disequilibrium can exist between the phases (groundmass and phenocrysts) of a single OIB lava. In this study, we target individual olivine-hosted melt inclusions from two samples—one Samoan and one Hawai'ian—with melt inclusion 87Sr/86Sr heterogeneity previously measured using laser ablation inductively coupled plasma mass spectrometry (LA-ICP-MS). We report 87Sr/86Sr and 143Nd/144Nd in individual melt inclusions analyzed by thermal ionization mass spectrometry (TIMS). In melt inclusions from Samoan sample AVON3-71-2, we find highly heterogeneous (935 ppm) 87Sr/86Sr (0.705193–0.705853, N = 6), consistent with previously identified 87Sr/86Sr heterogeneity (~2030 ppm) by laser ablation multi-collector ICP-MS (0.70459–0.70602, N = 12). In contrast, we find comparatively little (251 ppm) 87Sr/86Sr heterogeneity (0.703761–0.703938, N = 9) in olivine-hosted melt inclusions contained in a Hawaiian scoria clast from the Pu'u Wahi eruption (Mauna Loa). This result contrasts with a previous measurements by single-collector LA-ICP-MS that found highly heterogeneous (~8500 ppm) 87Sr/86Sr in olivine-hosted melt inclusions from the same eruption (0.7021–0.7081, N = 137). In both the AVON3-71-2 and Pu'u Wahi melt inclusions, 143Nd/144Nd is indistinguishable from their respective whole rock 143Nd/144Nd values. The isotopic measurements on the melt inclusions are paired with major and trace element concentrations to investigate the mechanisms generating 87Sr/86Sr variability in melt inclusions. The lack of significant 87Sr/86Sr variability in the Hawai'ian melt inclusions (only 251 ppm) from Pu'u Wahi suggests a relatively simple magmatic history. In contrast, for the Samoan melt inclusions, we present evidence that supports the mixing of isotopically-heterogeneous mantle-derived melts as the mechanism generating the observed 87Sr/86Sr and trace element variability in the melt inclusions from AVON3-71-2. However, brine interaction appears to have increased the Cl concentrations of some of the Samoan inclusions without significantly modifying the 87Sr/86Sr or the other elemental budgets examined in this study.\n

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\n \n\n \n \n \n \n \n \n A New, Long-lived, Jupiter Mesoscale Wave Observed at Visible Wavelengths.\n \n \n \n \n\n\n \n Simon, A. A.; Hueso, R.; Iñurrigarro, P.; Sánchez-Lavega, A.; Morales-Juberías, R.; Cosentino, R.; Fletcher, L. N.; Wong, M. H.; Hsu, A. I.; Pater, I. d.; Orton, G. S.; Colas, F.; Delcroix, M.; Peach, D.; and Gómez-Forrellad, J.\n\n\n \n\n\n\n The Astronomical Journal, 156(2): 79. August 2018.\n \n\n\n\n
\n\n\n\n \n \n $\"A$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{simon_new_2018,\n\ttitle = {A {New}, {Long}-lived, {Jupiter} {Mesoscale} {Wave} {Observed} at {Visible} {Wavelengths}},\n\tvolume = {156},\n\tissn = {1538-3881},\n\turl = {https://iopscience.iop.org/article/10.3847/1538-3881/aacaf5/meta},\n\tdoi = {10.3847/1538-3881/aacaf5},\n\tlanguage = {en},\n\tnumber = {2},\n\turldate = {2021-09-08},\n\tjournal = {The Astronomical Journal},\n\tauthor = {Simon, Amy A. and Hueso, Ricardo and Iñurrigarro, Peio and Sánchez-Lavega, Agustín and Morales-Juberías, Raúl and Cosentino, Richard and Fletcher, Leigh N. and Wong, Michael H. and Hsu, Andrew I. and Pater, Imke de and Orton, Glenn S. and Colas, François and Delcroix, Marc and Peach, Damian and Gómez-Forrellad, Josep-María},\n\tmonth = aug,\n\tyear = {2018},\n\tpages = {79},\n}\n\n

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\n \n\n \n \n \n \n \n \n Organic Aerosols in Anoxic and Oxic Atmospheres of Earth-like Exoplanets: VUV-MIR Spectroscopy of CHON Tholins.\n \n \n \n \n\n\n \n Gavilan, L.; Carrasco, N.; Hoffmann, S. V.; Jones, N. C.; and Mason, N. J.\n\n\n \n\n\n\n The Astrophysical Journal, 861(2): 110. July 2018.\n \n\n\n\n
\n\n\n\n \n \n $\"Organic$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{gavilan_organic_2018,\n\ttitle = {Organic {Aerosols} in {Anoxic} and {Oxic} {Atmospheres} of {Earth}-like {Exoplanets}: {VUV}-{MIR} {Spectroscopy} of {CHON} {Tholins}},\n\tvolume = {861},\n\tissn = {0004-637X},\n\tshorttitle = {Organic {Aerosols} in {Anoxic} and {Oxic} {Atmospheres} of {Earth}-like {Exoplanets}},\n\turl = {https://iopscience.iop.org/article/10.3847/1538-4357/aac8df/meta},\n\tdoi = {10.3847/1538-4357/aac8df},\n\tlanguage = {en},\n\tnumber = {2},\n\turldate = {2021-09-08},\n\tjournal = {The Astrophysical Journal},\n\tauthor = {Gavilan, Lisseth and Carrasco, Nathalie and Hoffmann, Søren Vrønning and Jones, Nykola C. and Mason, Nigel J.},\n\tmonth = jul,\n\tyear = {2018},\n\tpages = {110},\n}\n\n

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\n \n\n \n \n \n \n \n \n MarsTEM sensor simulations in Martian dust environment.\n \n \n \n \n\n\n \n Colombatti, G.; Bettanini, C.; Aboudan, A.; Debei, S.; Esposito, F.; Molfese, C.; Cecere, A.; Merrison, J.; and Iversen, J. J.\n\n\n \n\n\n\n Measurement, 122: 453–458. July 2018.\n \n\n\n\n
\n\n\n\n \n \n $\"MarsTEM$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{colombatti_marstem_2018,\n\ttitle = {{MarsTEM} sensor simulations in {Martian} dust environment},\n\tvolume = {122},\n\tissn = {0263-2241},\n\turl = {https://www.sciencedirect.com/science/article/pii/S026322411730814X},\n\tdoi = {10.1016/j.measurement.2017.12.043},\n\tabstract = {A wind tunnel test campaign has been conducted prior to the landing of the Exomars2016 EDM module on the Meridiani Planum on the 19th of October 2016. Test were performed in the Mars wind tunnel facility at Aahrus University (DK) under the 2015 Europlanet Call. The facility was available for a 5 days campaign where different environmental configurations were tested and both a full scale DREAMS (Dust Characterisation, Risk Assessment, and Environment Analyser on the Martian Surface) Metmast model and a Descent Module mockup were studied. In particular the MarsTEM (Mars TEMperature sensor), the temperature sensor of the DREAMS package onboard Exomars2016, was studied for different wind velocities and directions, effect of light sources and presence of dust. The test showed that the sensor response is dependent on wind direction but only slightly on wind velocities. It also seems that the presence of the dust in the wind and the consequent dust deposit on the Metmast and the sensor itself uniforms the response for different wind velocities and directions. Light is also affecting the measurements but it is still not so clear what will be the effect on Mars due to the particular light sources used for the test.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Measurement},\n\tauthor = {Colombatti, Giacomo and Bettanini, Carlo and Aboudan, Alessio and Debei, Stefano and Esposito, Francesca and Molfese, Cesare and Cecere, Anselmo and Merrison, John and Iversen, Jens Jacob},\n\tmonth = jul,\n\tyear = {2018},\n\tkeywords = {DREAMS, Exomars2016, MarsTEM, Wind tunnel chamber},\n\tpages = {453--458},\n}\n\n

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\n \n\n \n \n \n \n \n \n Quantifying the contact electrification of aerosolized insulating particles.\n \n \n \n \n\n\n \n Alois, S.; Merrison, J.; Iversen, J. J.; and Sesterhenn, J.\n\n\n \n\n\n\n Powder Technology, 332: 106–113. June 2018.\n \n\n\n\n
\n\n\n\n \n \n $\"Quantifying$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{alois_quantifying_2018,\n\ttitle = {Quantifying the contact electrification of aerosolized insulating particles},\n\tvolume = {332},\n\tissn = {0032-5910},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0032591018302523},\n\tdoi = {10.1016/j.powtec.2018.03.059},\n\tabstract = {The contact electrification of aerosolized micron-scale oxide particles has been investigated experimentally and the size and composition dependence determined. The net charge acquired by particles contacting the aerosolizer was seen to increase linearly with their surface area. A physically meaningful model based upon electron transfer has been applied leading to a predictive expression for the total particle surface charge concentration generated (σ) dependent on the absolute generalized relative electronegativity (χAGR); σ = aχAGR − b, where a = 4.7 e/μm2/V, b = −27 e/μm2 and χAGR is obtained by knowing the composition of the two contacting surfaces. The influence of relative humidity and particle cohesion on the contact electrification process was investigated. A maximum surface charge concentration of around 100 e/μm2 was found, in agreement with previous work.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Powder Technology},\n\tauthor = {Alois, Stefano and Merrison, Jonathan and Iversen, Jens Jacob and Sesterhenn, Jörn},\n\tmonth = jun,\n\tyear = {2018},\n\tkeywords = {Aerosol, Contact electrification, Electronegativity, Insulating particles, Tribo-electrification},\n\tpages = {106--113},\n}\n\n

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\n \n\n \n \n \n \n \n \n Statistical Analysis of Solar Events Associated with Storm Sudden Commencements over One Year of Solar Maximum During Cycle 23: Propagation from the Sun to the Earth and Effects.\n \n \n \n \n\n\n \n Bocchialini, K.; Grison, B.; Menvielle, M.; Chambodut, A.; Cornilleau-Wehrlin, N.; Fontaine, D.; Marchaudon, A.; Pick, M.; Pitout, F.; Schmieder, B.; Régnier, S.; and Zouganelis, I.\n\n\n \n\n\n\n Solar Physics, 293(5): 75. April 2018.\n \n\n\n\n
\n\n\n\n \n \n $\"Statistical$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{bocchialini_statistical_2018,\n\ttitle = {Statistical {Analysis} of {Solar} {Events} {Associated} with {Storm} {Sudden} {Commencements} over {One} {Year} of {Solar} {Maximum} {During} {Cycle} 23: {Propagation} from the {Sun} to the {Earth} and {Effects}},\n\tvolume = {293},\n\tissn = {1573-093X},\n\tshorttitle = {Statistical {Analysis} of {Solar} {Events} {Associated} with {Storm} {Sudden} {Commencements} over {One} {Year} of {Solar} {Maximum} {During} {Cycle} 23},\n\turl = {https://doi.org/10.1007/s11207-018-1278-5},\n\tdoi = {10.1007/s11207-018-1278-5},\n\tabstract = {Taking the 32 storm sudden commencements (SSCs) listed by the International Service of Geomagnetic Indices (ISGI) of the Observatory de l’Ebre during 2002 (solar activity maximum in Cycle 23) as a starting point, we performed a multi-criterion analysis based on observations (propagation time, velocity comparisons, sense of the magnetic field rotation, radio waves) to associate them with solar sources, identified their effects in the interplanetary medium, and looked at the response of the terrestrial ionized and neutral environment. We find that 28 SSCs can be related to 44 coronal mass ejections (CMEs), 15 with a unique CME and 13 with a series of multiple CMEs, among which 19 (68\\%) involved halo CMEs. Twelve of the 19 fastest CMEs with speeds greater than 1000 km s−1 are halo CMEs. For the 44 CMEs, including 21 halo CMEs, the corresponding X-ray flare classes are: 3 X-class, 19 M-class, and 22 C-class flares. The probability for an SSC to occur is 75\\% if the CME is a halo CME. Among the 500, or even more, front-side, non-halo CMEs recorded in 2002, only 23 could be the source of an SSC, i.e. 5\\%. The complex interactions between two (or more) CMEs and the modification of their trajectories have been examined using joint white-light and multiple-wavelength radio observations. The detection of long-lasting type IV bursts observed at metric–hectometric wavelengths is a very useful criterion for the CME–SSC events association. The events associated with the most depressed Dst values are also associated with type IV radio bursts. The four SSCs associated with a single shock at L1 correspond to four radio events exhibiting characteristics different from type IV radio bursts. The solar-wind structures at L1 after the 32 SSCs are 12 magnetic clouds (MCs), 6 interplanetary coronal mass ejections (ICMEs) without an MC structure, 4 miscellaneous structures, which cannot unambiguously be classified as ICMEs, 5 corotating or stream interaction regions (CIRs/SIRs), one CIR caused two SSCs, and 4 shock events; note than one CIR caused two SSCs. The 11 MCs listed in 3 or more MC catalogs covering the year 2002 are associated with SSCs. For the three most intense geomagnetic storms (based on Dst minima) related to MCs, we note two sudden increases of the Dst, at the arrival of the sheath and the arrival of the MC itself. In terms of geoeffectiveness, the relation between the CME speed and the magnetic-storm intensity, as characterized using the Dst magnetic index, is very complex, but generally CMEs with velocities at the Sun larger than 1000 km s−1 have larger probabilities to trigger moderate or intense storms. The most geoeffective events are MCs, since 92\\% of them trigger moderate or intense storms, followed by ICMEs (33\\%). At best, CIRs/SIRs only cause weak storms. We show that these geoeffective events (ICMEs or MCs) trigger an increased and combined auroral kilometric radiation (AKR) and non-thermal continuum (NTC) wave activity in the magnetosphere, an enhanced convection in the ionosphere, and a stronger response in the thermosphere. However, this trend does not appear clearly in the coupling functions, which exhibit relatively weak correlations between the solar-wind energy input and the amplitude of various geomagnetic indices, whereas the role of the southward component of the solar-wind magnetic field is confirmed. Some saturation appears for Dst values \\${\\textless} -100\\$ nT on the integrated values of the polar and auroral indices.},\n\tlanguage = {en},\n\tnumber = {5},\n\turldate = {2021-09-08},\n\tjournal = {Solar Physics},\n\tauthor = {Bocchialini, K. and Grison, B. and Menvielle, M. and Chambodut, A. and Cornilleau-Wehrlin, N. and Fontaine, D. and Marchaudon, A. and Pick, M. and Pitout, F. and Schmieder, B. and Régnier, S. and Zouganelis, I.},\n\tmonth = apr,\n\tyear = {2018},\n\tpages = {75},\n}\n\n

\n\n\n

\n Taking the 32 storm sudden commencements (SSCs) listed by the International Service of Geomagnetic Indices (ISGI) of the Observatory de l’Ebre during 2002 (solar activity maximum in Cycle 23) as a starting point, we performed a multi-criterion analysis based on observations (propagation time, velocity comparisons, sense of the magnetic field rotation, radio waves) to associate them with solar sources, identified their effects in the interplanetary medium, and looked at the response of the terrestrial ionized and neutral environment. We find that 28 SSCs can be related to 44 coronal mass ejections (CMEs), 15 with a unique CME and 13 with a series of multiple CMEs, among which 19 (68%) involved halo CMEs. Twelve of the 19 fastest CMEs with speeds greater than 1000 km s−1 are halo CMEs. For the 44 CMEs, including 21 halo CMEs, the corresponding X-ray flare classes are: 3 X-class, 19 M-class, and 22 C-class flares. The probability for an SSC to occur is 75% if the CME is a halo CME. Among the 500, or even more, front-side, non-halo CMEs recorded in 2002, only 23 could be the source of an SSC, i.e. 5%. The complex interactions between two (or more) CMEs and the modification of their trajectories have been examined using joint white-light and multiple-wavelength radio observations. The detection of long-lasting type IV bursts observed at metric–hectometric wavelengths is a very useful criterion for the CME–SSC events association. The events associated with the most depressed Dst values are also associated with type IV radio bursts. The four SSCs associated with a single shock at L1 correspond to four radio events exhibiting characteristics different from type IV radio bursts. The solar-wind structures at L1 after the 32 SSCs are 12 magnetic clouds (MCs), 6 interplanetary coronal mass ejections (ICMEs) without an MC structure, 4 miscellaneous structures, which cannot unambiguously be classified as ICMEs, 5 corotating or stream interaction regions (CIRs/SIRs), one CIR caused two SSCs, and 4 shock events; note than one CIR caused two SSCs. The 11 MCs listed in 3 or more MC catalogs covering the year 2002 are associated with SSCs. For the three most intense geomagnetic storms (based on Dst minima) related to MCs, we note two sudden increases of the Dst, at the arrival of the sheath and the arrival of the MC itself. In terms of geoeffectiveness, the relation between the CME speed and the magnetic-storm intensity, as characterized using the Dst magnetic index, is very complex, but generally CMEs with velocities at the Sun larger than 1000 km s−1 have larger probabilities to trigger moderate or intense storms. The most geoeffective events are MCs, since 92% of them trigger moderate or intense storms, followed by ICMEs (33%). At best, CIRs/SIRs only cause weak storms. We show that these geoeffective events (ICMEs or MCs) trigger an increased and combined auroral kilometric radiation (AKR) and non-thermal continuum (NTC) wave activity in the magnetosphere, an enhanced convection in the ionosphere, and a stronger response in the thermosphere. However, this trend does not appear clearly in the coupling functions, which exhibit relatively weak correlations between the solar-wind energy input and the amplitude of various geomagnetic indices, whereas the role of the southward component of the solar-wind magnetic field is confirmed. Some saturation appears for Dst values ${\\textless} -100$ nT on the integrated values of the polar and auroral indices.\n

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\n \n\n \n \n \n \n \n \n Can we make a case for astronomy?.\n \n \n \n \n\n\n \n Heward, A.; and Massey, R.\n\n\n \n\n\n\n Astronomy & Geophysics, 59(1): 1.27–1.29. February 2018.\n \n\n\n\n
\n\n\n\n \n \n $\"Can$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{heward_can_2018,\n\ttitle = {Can we make a case for astronomy?},\n\tvolume = {59},\n\tissn = {1366-8781},\n\turl = {https://doi.org/10.1093/astrogeo/aty027},\n\tdoi = {10.1093/astrogeo/aty027},\n\tabstract = {Anita Heward and Robert Massey report from a meeting that discussed how astronomers could engage with the public and politicians – and ask what are the most effective ways to do so?},\n\tnumber = {1},\n\turldate = {2021-09-08},\n\tjournal = {Astronomy \\& Geophysics},\n\tauthor = {Heward, Anita and Massey, Robert},\n\tmonth = feb,\n\tyear = {2018},\n\tpages = {1.27--1.29},\n}\n\n

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\n \n\n \n \n \n \n \n \n Redescription of Dexiotricha colpidiopsis (Kahl, 1926) Jankowski, 1964 (Ciliophora, Oligohymenophorea) from a Hot Spring in Iceland with Identification Key for Dexiotricha species.\n \n \n \n \n\n\n \n Qu, Z.; Groben, R.; Marteinsson, V.; Agatha, S.; Filker, S.; and Stoeck, T.\n\n\n \n\n\n\n Acta Protozoologica, 2018(Volume 57, Issue 2): 95–106. December 2018.\n \n\n\n\n
\n\n\n\n \n \n $\"Redescription$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{qu_redescription_2018,\n\ttitle = {Redescription of {Dexiotricha} colpidiopsis ({Kahl}, 1926) {Jankowski}, 1964 ({Ciliophora}, {Oligohymenophorea}) from a {Hot} {Spring} in {Iceland} with {Identification} {Key} for {Dexiotricha} species},\n\tvolume = {2018},\n\tissn = {1689-0027},\n\turl = {https://www.ejournals.eu/Acta-Protozoologica/2018/Issue-2/art/13131/},\n\tdoi = {10.4467/16890027AP.18.009.8983},\n\tabstract = {{\\textless}div id="cke\\_pastebin"{\\textgreater}\n\tRedescription of Dexiotricha colpidiopsis (Kahl, 1926) Jankowski, 1964 (Ciliophora, Oligohymenophorea) from a Hot Spring in Iceland with Identification Key for Dexiotricha species{\\textless}/div{\\textgreater}},\n\tlanguage = {en},\n\tnumber = {Volume 57, Issue 2},\n\turldate = {2021-09-08},\n\tjournal = {Acta Protozoologica},\n\tauthor = {Qu, Zhishuai and Groben, René and Marteinsson, Viggó and Agatha, Sabine and Filker, Sabine and Stoeck, Thorsten},\n\tmonth = dec,\n\tyear = {2018},\n\tpages = {95--106},\n}\n\n

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\n \n\n \n \n \n \n \n \n The Planetary Spectroscopy Laboratory (PSL): wide spectral range, wider sample temperature range.\n \n \n \n \n\n\n \n Maturilli, A.; Helbert, J.; D'Amore, M.; Varatharajan, I.; and Ortiz, Y. R.\n\n\n \n\n\n\n In Infrared Remote Sensing and Instrumentation XXVI, volume 10765, pages 107650A, September 2018. International Society for Optics and Photonics\n \n\n\n\n
\n\n\n\n \n \n $\"The$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@inproceedings{maturilli_planetary_2018,\n\ttitle = {The {Planetary} {Spectroscopy} {Laboratory} ({PSL}): wide spectral range, wider sample temperature range},\n\tvolume = {10765},\n\tshorttitle = {The {Planetary} {Spectroscopy} {Laboratory} ({PSL})},\n\turl = {https://www.spiedigitallibrary.org/conference-proceedings-of-spie/10765/107650A/The-Planetary-Spectroscopy-Laboratory-PSL--wide-spectral-range-wider/10.1117/12.2319944.short},\n\tdoi = {10.1117/12.2319944},\n\tabstract = {The Planetary Spectroscopy Laboratory (PSL) of DLR in Berlin provides spectral measurements of primarily planetary analogues from the visible to the far-infrared range. PSL has supported the data analysis as well as the development and calibration of instruments for planetary missions from ESA, NASA and JAXA. For this purposes PSL provides reflection, transmission and emission spectroscopy of target materials. Currently PSL operates two identical Bruker Vertex 80V vacuum FTIR spectrometer, one spectrometer is equipped with aluminum mirrors optimized for the UV, visible and near-IR, the second features gold-coated mirrors for the near to far IR spectral range. External simulation chambers are attached to each of the instruments for emissivity measurements. The chamber at the near to far IR instruments allows emissivity measurements from 0.7-200 \\&mu;m under vacuum for sample temperatures from 320K to above 900K, using an innovative induction system. The second chamber (purged with dry air and water cooled to \\&le;270K) allows emissivity measurements of samples with surface temperature from 290 to 420K. We measure bi-directional reflectance of samples, with variable incidence and emission angles between 13\\&deg; and 85\\&deg;. Samples are measured currently at room temperature and 170K, with a planned extension for temperatures below 100K. Bi-directional and hemispherical reflectance is measured under purging/vacuum conditions, covering the 0.2 to above 200 \\&mu;m spectral range. Transmission of thin slabs, optical filters, optical windows, pellets, and others is measured in the complete spectral range from UV to FIR using a parallel beam configuration to avoid refraction.},\n\turldate = {2021-09-08},\n\tbooktitle = {Infrared {Remote} {Sensing} and {Instrumentation} {XXVI}},\n\tpublisher = {International Society for Optics and Photonics},\n\tauthor = {Maturilli, A. and Helbert, J. and D'Amore, M. and Varatharajan, I. and Ortiz, Y. Rosas},\n\tmonth = sep,\n\tyear = {2018},\n\tpages = {107650A},\n}\n\n

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\n \n\n \n \n \n \n \n \n Transitory microbial habitat in the hyperarid Atacama Desert.\n \n \n \n \n\n\n \n Schulze-Makuch, D.; Wagner, D.; Kounaves, S. P.; Mangelsdorf, K.; Devine, K. G.; Vera, J. d.; Schmitt-Kopplin, P.; Grossart, H.; Parro, V.; Kaupenjohann, M.; Galy, A.; Schneider, B.; Airo, A.; Frösler, J.; Davila, A. F.; Arens, F. L.; Cáceres, L.; Cornejo, F. S.; Carrizo, D.; Dartnell, L.; DiRuggiero, J.; Flury, M.; Ganzert, L.; Gessner, M. O.; Grathwohl, P.; Guan, L.; Heinz, J.; Hess, M.; Keppler, F.; Maus, D.; McKay, C. P.; Meckenstock, R. U.; Montgomery, W.; Oberlin, E. A.; Probst, A. J.; Sáenz, J. S.; Sattler, T.; Schirmack, J.; Sephton, M. A.; Schloter, M.; Uhl, J.; Valenzuela, B.; Vestergaard, G.; Wörmer, L.; and Zamorano, P.\n\n\n \n\n\n\n Proceedings of the National Academy of Sciences, 115(11): 2670–2675. March 2018.\n \n\n\n\n
\n\n\n\n \n \n $\"Transitory$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{schulze-makuch_transitory_2018,\n\ttitle = {Transitory microbial habitat in the hyperarid {Atacama} {Desert}},\n\tvolume = {115},\n\tcopyright = {Copyright © 2018 the Author(s). Published by PNAS.. https://creativecommons.org/licenses/by-nc-nd/4.0/This open access article is distributed under Creative Commons Attribution-NonCommercial-NoDerivatives License 4.0 (CC BY-NC-ND).},\n\tissn = {0027-8424, 1091-6490},\n\turl = {https://www.pnas.org/content/115/11/2670},\n\tdoi = {10.1073/pnas.1714341115},\n\tabstract = {Traces of life are nearly ubiquitous on Earth. However, a central unresolved question is whether these traces always indicate an active microbial community or whether, in extreme environments, such as hyperarid deserts, they instead reflect just dormant or dead cells. Although microbial biomass and diversity decrease with increasing aridity in the Atacama Desert, we provide multiple lines of evidence for the presence of an at times metabolically active, microbial community in one of the driest places on Earth. We base this observation on four major lines of evidence: (i) a physico-chemical characterization of the soil habitability after an exceptional rain event, (ii) identified biomolecules indicative of potentially active cells [e.g., presence of ATP, phospholipid fatty acids (PLFAs), metabolites, and enzymatic activity], (iii) measurements of in situ replication rates of genomes of uncultivated bacteria reconstructed from selected samples, and (iv) microbial community patterns specific to soil parameters and depths. We infer that the microbial populations have undergone selection and adaptation in response to their specific soil microenvironment and in particular to the degree of aridity. Collectively, our results highlight that even the hyperarid Atacama Desert can provide a habitable environment for microorganisms that allows them to become metabolically active following an episodic increase in moisture and that once it decreases, so does the activity of the microbiota. These results have implications for the prospect of life on other planets such as Mars, which has transitioned from an earlier wetter environment to today’s extreme hyperaridity.},\n\tlanguage = {en},\n\tnumber = {11},\n\turldate = {2021-09-08},\n\tjournal = {Proceedings of the National Academy of Sciences},\n\tauthor = {Schulze-Makuch, Dirk and Wagner, Dirk and Kounaves, Samuel P. and Mangelsdorf, Kai and Devine, Kevin G. and Vera, Jean-Pierre de and Schmitt-Kopplin, Philippe and Grossart, Hans-Peter and Parro, Victor and Kaupenjohann, Martin and Galy, Albert and Schneider, Beate and Airo, Alessandro and Frösler, Jan and Davila, Alfonso F. and Arens, Felix L. and Cáceres, Luis and Cornejo, Francisco Solís and Carrizo, Daniel and Dartnell, Lewis and DiRuggiero, Jocelyne and Flury, Markus and Ganzert, Lars and Gessner, Mark O. and Grathwohl, Peter and Guan, Lisa and Heinz, Jacob and Hess, Matthias and Keppler, Frank and Maus, Deborah and McKay, Christopher P. and Meckenstock, Rainer U. and Montgomery, Wren and Oberlin, Elizabeth A. and Probst, Alexander J. and Sáenz, Johan S. and Sattler, Tobias and Schirmack, Janosch and Sephton, Mark A. and Schloter, Michael and Uhl, Jenny and Valenzuela, Bernardita and Vestergaard, Gisle and Wörmer, Lars and Zamorano, Pedro},\n\tmonth = mar,\n\tyear = {2018},\n\tpmid = {29483268},\n\tkeywords = {Mars, aridity, biomarker, habitat, microbial activity},\n\tpages = {2670--2675},\n}\n\n

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\n \n\n \n \n \n \n \n \n VNIR Reflectance Spectra of Mirabilite (Na2SO4 •10H2O) with 3 Different Grain Sizes and at Variable Temperature (80-298K).\n \n \n \n \n\n\n \n De Angelis, S.; Tosi, F.; Carli, C.; Beck, P.; Brissaud, O.; and Schmitt, B.\n\n\n \n\n\n\n 2018.\n \n\n\n\n
\n\n\n\n \n \n $\"VNIR$ Paper\n \n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@misc{de_angelis_vnir_2018,\n\ttitle = {{VNIR} {Reflectance} {Spectra} of {Mirabilite} ({Na2SO4} •{10H2O}) with 3 {Different} {Grain} {Sizes} and at {Variable} {Temperature} (80-{298K})},\n\turl = {https://doi.org/10.26302/SSHADE/EXPERIMENT_CC_20180428_002},\n\tlanguage = {en},\n\tpublisher = {SSHADE/REFL\\_SLAB+CSS (OSUG Data Center)},\n\tauthor = {De Angelis, Simone and Tosi, Federico and Carli, Cristian and Beck, Pierre and Brissaud, Olivier and Schmitt, Bernard},\n\tyear = {2018},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n VNIR Reflectance Spectra of Thénardite (Na2SO4) with 3 Different Grain Sizes and at Variable Temperature (80-304K).\n \n \n \n \n\n\n \n De Angelis, S.; Tosi, F.; Carli, C.; Beck, P.; Brissaud, O.; and Schmitt, B.\n\n\n \n\n\n\n 2018.\n \n\n\n\n
\n\n\n\n \n \n $\"VNIR$ Paper\n \n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@misc{de_angelis_vnir_2018-1,\n\ttitle = {{VNIR} {Reflectance} {Spectra} of {Thénardite} ({Na2SO4}) with 3 {Different} {Grain} {Sizes} and at {Variable} {Temperature} (80-{304K}).},\n\turl = {https://doi.org/10.26302/SSHADE/EXPERIMENT_CC_20180427_001},\n\tlanguage = {en},\n\tpublisher = {SSHADE/REFL\\_SLAB+CSS (OSUG Data Center)},\n\tauthor = {De Angelis, Simone and Tosi, Federico and Carli, Cristian and Beck, Pierre and Brissaud, Olivier and Schmitt, Bernard},\n\tyear = {2018},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Temperature-dependent VNIR spectroscopy of thénardite and mirabilite.\n \n \n \n \n\n\n \n Tosi, F.; De Angelis, S.; Carli, C.; Beck, P.; Potin, S.; Brissaud, O.; Schmitt, B.; and Piccioni, G.\n\n\n \n\n\n\n ,EPSC2018–550. September 2018.\n \n\n\n\n
\n\n\n\n \n \n $\"Temperature-dependent$ Paper\n \n \n\n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{tosi_temperature-dependent_2018,\n\ttitle = {Temperature-dependent {VNIR} spectroscopy of thénardite and mirabilite},\n\turl = {https://ui.adsabs.harvard.edu/abs/2018EPSC...12..550T},\n\tabstract = {In the framework of the EuroPlanet 2020 Research Infrastructure (RI) programme, we took advantage of the CSS distributed planetary simulation facility at IPAG-Grenoble to perform a series of laboratory measurements aimed to acquire VIS-NIR spectra of anhydrous sodium sulfate (thénardite) and sodium sulfate decahydrate (mirabilite), in three different grain sizes and in a broad range of cryogenic temperatures, representative of real planetary surfaces. These measurements are key to correctly interpret data acquired by spectrometers carried onboard ongoing and future interplanetary space missions aimed at various planetary bodies, particularly the Jovian icy satellites (JUICE, Europa Clipper) and Mars (ExoMars 2020, Mars 2020).},\n\tlanguage = {en},\n\turldate = {2021-07-26},\n\tauthor = {Tosi, Federico and De Angelis, Simone and Carli, Cristian and Beck, Pierre and Potin, Sandra and Brissaud, Olivier and Schmitt, Bernard and Piccioni, Giuseppe},\n\tmonth = sep,\n\tyear = {2018},\n\tpages = {EPSC2018--550},\n}\n\n

\n\n\n\n\n\n

\n\n

\n \n 2017\n \n \n (9)\n \n \n

\n \n \n

\n \n\n \n \n \n \n \n \n Rosetta Mission: Electron Scattering Cross Sections—Data Needs and Coverage in BEAMDB Database.\n \n \n \n \n\n\n \n Marinković, B. P.; Bredehöft, J. H.; Vujčić, V.; Jevremović, D.; and Mason, N. J.\n\n\n \n\n\n\n Atoms, 5(4): 46. December 2017.\n \n\n\n\n
\n\n\n\n \n \n $\"Rosetta$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{marinkovic_rosetta_2017,\n\ttitle = {Rosetta {Mission}: {Electron} {Scattering} {Cross} {Sections}—{Data} {Needs} and {Coverage} in {BEAMDB} {Database}},\n\tvolume = {5},\n\tcopyright = {http://creativecommons.org/licenses/by/3.0/},\n\tshorttitle = {Rosetta {Mission}},\n\turl = {https://www.mdpi.com/2218-2004/5/4/46},\n\tdoi = {10.3390/atoms5040046},\n\tabstract = {The emission of [O I] lines in the coma of Comet 67P/Churyumov-Gerasimenko during the Rosetta mission have been explained by electron impact dissociation of water rather than the process of photodissociation. This is the direct evidence for the role of electron induced processing has been seen on such a body. Analysis of other emission features is handicapped by a lack of detailed knowledge of electron impact cross sections which highlights the need for a broad range of electron scattering data from the molecular systems detected on the comet. In this paper, we present an overview of the needs for electron scattering data relevant for the understanding of observations in coma, the tenuous atmosphere and on the surface of 67P/Churyumov-Gerasimenko during the Rosetta mission. The relevant observations for elucidating the role of electrons come from optical spectra, particle analysis using the ion and electron sensors and mass spectrometry measurements. To model these processes electron impact data should be collated and reviewed in an electron scattering database and an example is given in the BEAMD, which is a part of a larger consortium of Virtual Atomic and Molecular Data Centre—VAMDC.},\n\tlanguage = {en},\n\tnumber = {4},\n\turldate = {2021-09-08},\n\tjournal = {Atoms},\n\tauthor = {Marinković, Bratislav P. and Bredehöft, Jan Hendrik and Vujčić, Veljko and Jevremović, Darko and Mason, Nigel J.},\n\tmonth = dec,\n\tyear = {2017},\n\tkeywords = {Rosetta mission, atomic and molecular databases, cross sections, electron scattering},\n\tpages = {46},\n}\n\n

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\n \n\n \n \n \n \n \n \n Water induced sediment levitation enhances downslope transport on Mars.\n \n \n \n \n\n\n \n Raack, J.; Conway, S. J.; Herny, C.; Balme, M. R.; Carpy, S.; and Patel, M. R.\n\n\n \n\n\n\n Nature Communications, 8(1): 1151. October 2017.\n \n\n\n\n
\n\n\n\n \n \n $\"Water$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{raack_water_2017,\n\ttitle = {Water induced sediment levitation enhances downslope transport on {Mars}},\n\tvolume = {8},\n\tcopyright = {2017 The Author(s)},\n\tissn = {2041-1723},\n\turl = {https://www.nature.com/articles/s41467-017-01213-z},\n\tdoi = {10.1038/s41467-017-01213-z},\n\tabstract = {On Mars, locally warm surface temperatures ({\\textasciitilde}293 K) occur, leading to the possibility of (transient) liquid water on the surface. However, water exposed to the martian atmosphere will boil, and the sediment transport capacity of such unstable water is not well understood. Here, we present laboratory studies of a newly recognized transport mechanism: “levitation” of saturated sediment bodies on a cushion of vapor released by boiling. Sediment transport where this mechanism is active is about nine times greater than without this effect, reducing the amount of water required to transport comparable sediment volumes by nearly an order of magnitude. Our calculations show that the effect of levitation could persist up to {\\textasciitilde}48 times longer under reduced martian gravity. Sediment levitation must therefore be considered when evaluating the formation of recent and present-day martian mass wasting features, as much less water may be required to form such features than previously thought.},\n\tlanguage = {en},\n\tnumber = {1},\n\turldate = {2021-09-08},\n\tjournal = {Nature Communications},\n\tauthor = {Raack, Jan and Conway, Susan J. and Herny, Clémence and Balme, Matthew R. and Carpy, Sabrina and Patel, Manish R.},\n\tmonth = oct,\n\tyear = {2017},\n\tpages = {1151},\n}\n\n

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\n \n\n \n \n \n \n \n \n Archaean and Proterozoic diamond growth from contrasting styles of large-scale magmatism.\n \n \n \n \n\n\n \n Koornneef, J. M.; Gress, M. U.; Chinn, I. L.; Jelsma, H. A.; Harris, J. W.; and Davies, G. R.\n\n\n \n\n\n\n Nature Communications, 8(1): 648. September 2017.\n \n\n\n\n
\n\n\n\n \n \n $\"Archaean$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{koornneef_archaean_2017,\n\ttitle = {Archaean and {Proterozoic} diamond growth from contrasting styles of large-scale magmatism},\n\tvolume = {8},\n\tcopyright = {2017 The Author(s)},\n\tissn = {2041-1723},\n\turl = {https://www.nature.com/articles/s41467-017-00564-x},\n\tdoi = {10.1038/s41467-017-00564-x},\n\tabstract = {Precise dating of diamond growth is required to understand the interior workings of the early Earth and the deep carbon cycle. Here we report Sm-Nd isotope data from 26 individual garnet inclusions from 26 harzburgitic diamonds from Venetia, South Africa. Garnet inclusions and host diamonds comprise two compositional suites formed under markedly different conditions and define two isochrons, one Archaean (2.95 Ga) and one Proterozoic (1.15 Ga). The Archaean diamond suite formed from relatively cool fluid-dominated metasomatism during rifting of the southern shelf of the Zimbabwe Craton. The 1.8 billion years younger Proterozoic diamond suite formed by melt-dominated metasomatism related to the 1.1 Ga Umkondo Large Igneous Province. The results demonstrate that resolving the time of diamond growth events requires dating of individual inclusions, and that there was a major change in the magmatic processes responsible for harzburgitic diamond formation beneath Venetia from the Archaean to the Proterozoic.},\n\tlanguage = {en},\n\tnumber = {1},\n\turldate = {2021-09-08},\n\tjournal = {Nature Communications},\n\tauthor = {Koornneef, Janne M. and Gress, Michael U. and Chinn, Ingrid L. and Jelsma, Hielke A. and Harris, Jeff W. and Davies, Gareth R.},\n\tmonth = sep,\n\tyear = {2017},\n\tpages = {648},\n}\n\n

\n\n\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n “Non-invasive” portable laser ablation sampling of art and archaeological materials with subsequent Sr–Nd isotope analysis by TIMS using 1013 Ω amplifiers.\n \n \n \n \n\n\n \n Knaf, A. C. S.; Koornneef, J. M.; and Davies, G. R.\n\n\n \n\n\n\n Journal of Analytical Atomic Spectrometry, 32(11): 2210–2216. November 2017.\n \n\n\n\n
\n\n\n\n \n \n $\"“Non-invasive”$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{knaf_non-invasive_2017,\n\ttitle = {“{Non}-invasive” portable laser ablation sampling of art and archaeological materials with subsequent {Sr}–{Nd} isotope analysis by {TIMS} using 1013 Ω amplifiers},\n\tvolume = {32},\n\tissn = {1364-5544},\n\turl = {https://pubs.rsc.org/en/content/articlelanding/2017/ja/c7ja00191f},\n\tdoi = {10.1039/C7JA00191F},\n\tabstract = {A new integrated trace element and multi-isotope provenancing methodology is presented that uses a portable “non-invasive” pulsed laser ablation sampling technique. Samples are collected on location onto Teflon filters for return to a clean laboratory for low blank (pg) geochemical procedures. Ablation pits approximately 60 or 120 μm in width and depth remove μg amounts of material. Following dissolution, trace element ratios are determined by inductively coupled plasma mass spectrometry and combined Sr–Nd isotopes by thermal ionization mass spectrometry. Use of 1013 Ω resistors allows precise analysis of subnanogram amounts of Sr–Nd isotopes, which coupled with the trace element data, provides highly effective multi-variant discrimination for material provenance and authenticity verification. Monitoring of blank contributions is required.},\n\tlanguage = {en},\n\tnumber = {11},\n\turldate = {2021-09-08},\n\tjournal = {Journal of Analytical Atomic Spectrometry},\n\tauthor = {Knaf, A. C. S. and Koornneef, J. M. and Davies, G. R.},\n\tmonth = nov,\n\tyear = {2017},\n\tpages = {2210--2216},\n}\n\n

\n\n\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n A propagation tool to connect remote-sensing observations with in-situ measurements of heliospheric structures.\n \n \n \n \n\n\n \n Rouillard, A. P.; Lavraud, B.; Génot, V.; Bouchemit, M.; Dufourg, N.; Plotnikov, I.; Pinto, R. F.; Sanchez-Diaz, E.; Lavarra, M.; Penou, M.; Jacquey, C.; André, N.; Caussarieu, S.; Toniutti, J. -.; Popescu, D.; Buchlin, E.; Caminade, S.; Alingery, P.; Davies, J. A.; Odstrcil, D.; and Mays, L.\n\n\n \n\n\n\n Planetary and Space Science, 147: 61–77. November 2017.\n \n\n\n\n
\n\n\n\n \n \n $\"A$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{rouillard_propagation_2017,\n\ttitle = {A propagation tool to connect remote-sensing observations with in-situ measurements of heliospheric structures},\n\tvolume = {147},\n\tissn = {0032-0633},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0032063316304664},\n\tdoi = {10.1016/j.pss.2017.07.001},\n\tabstract = {The remoteness of the Sun and the harsh conditions prevailing in the solar corona have so far limited the observational data used in the study of solar physics to remote-sensing observations taken either from the ground or from space. In contrast, the ‘solar wind laboratory’ is directly measured in situ by a fleet of spacecraft measuring the properties of the plasma and magnetic fields at specific points in space. Since 2007, the solar-terrestrial relations observatory (STEREO) has been providing images of the solar wind that flows between the solar corona and spacecraft making in-situ measurements. This has allowed scientists to directly connect processes imaged near the Sun with the subsequent effects measured in the solar wind. This new capability prompted the development of a series of tools and techniques to track heliospheric structures through space. This article presents one of these tools, a web-based interface called the ’Propagation Tool’ that offers an integrated research environment to study the evolution of coronal and solar wind structures, such as Coronal Mass Ejections (CMEs), Corotating Interaction Regions (CIRs) and Solar Energetic Particles (SEPs). These structures can be propagated from the Sun outwards to or alternatively inwards from planets and spacecraft situated in the inner and outer heliosphere. In this paper, we present the global architecture of the tool, discuss some of the assumptions made to simulate the evolution of the structures and show how the tool connects to different databases.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Planetary and Space Science},\n\tauthor = {Rouillard, A. P. and Lavraud, B. and Génot, V. and Bouchemit, M. and Dufourg, N. and Plotnikov, I. and Pinto, R. F. and Sanchez-Diaz, E. and Lavarra, M. and Penou, M. and Jacquey, C. and André, N. and Caussarieu, S. and Toniutti, J. -P. and Popescu, D. and Buchlin, E. and Caminade, S. and Alingery, P. and Davies, J. A. and Odstrcil, D. and Mays, L.},\n\tmonth = nov,\n\tyear = {2017},\n\tkeywords = {CIRs, CMEs, Heliophysics, Solar imaging},\n\tpages = {61--77},\n}\n\n

\n\n\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n The influence of human exploration on the microbial community structure and ammonia oxidizing potential of the Su Bentu limestone cave in Sardinia, Italy.\n \n \n \n \n\n\n \n Leuko, S.; Koskinen, K.; Sanna, L.; D’Angeli, I. M.; Waele, J. D.; Marcia, P.; Moissl-Eichinger, C.; and Rettberg, P.\n\n\n \n\n\n\n PLOS ONE, 12(7): e0180700. July 2017.\n \n\n\n\n
\n\n\n\n \n \n $\"The$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{leuko_influence_2017,\n\ttitle = {The influence of human exploration on the microbial community structure and ammonia oxidizing potential of the {Su} {Bentu} limestone cave in {Sardinia}, {Italy}},\n\tvolume = {12},\n\tissn = {1932-6203},\n\turl = {https://journals.plos.org/plosone/article?id=10.1371/journal.pone.0180700},\n\tdoi = {10.1371/journal.pone.0180700},\n\tabstract = {The bacterial diversity in the Su Bentu Cave in Sardinia was investigated by means of 16S rRNA gene-based analysis. This 15 km long cave, carved in Jurassic limestone, hosts a variety of calcite speleothems, and a long succession of subterranean lakes with mixed granite and carbonate sands. The lower level is occasionally flooded by a rising groundwater level, but with only scarce input of organic remains (leaves and charcoal fragments). On the quiet cave pools there are visible calcite rafts, whereas walls are locally coated with manganese deposits. In the drier upper levels, where organic input is much more subdued, moonmilk—a hydrated calcium-magnesium carbonate speleothem—can be found. Relative humidity approaches 100\\% and the measured mean annual cave air temperature is 14.8°C. Samples were obtained in 2014 from calcite rafts, moonmilk, manganese oxide deposits and soil (limestone and granite grains). Microclimatic conditions in the cave near the sampling sites, sample properties, physico-chemical parameters of water, and sediment composition were determined. The microbial community of this system is predominately composed of the phyla Proteobacteria, Actinobacteria, Acidobacteria, Nitrospirae, and Firmicutes. Sampling sites near the entrance of the cave and in close proximity of the underground campsite–located 500 meters deep into the cave—revealed the highest diversity as well as the highest number of human associated microorganisms. Two samples obtained in very close proximity of each other near the campsite, indicate that the human impact is localized and is not distributed freely within the system. Analysis of the abundance of bacterial and archaeal amoA genes revealed a far greater abundance of archaeal amoA genes compared to bacterial representatives. The results of this study highlight that human impact is confined to locations that are utilized as campsites and that exploration leaves little microbial trails. Furthermore, we uncovered a highly specialized microbiome, which is perfectly adapted to survive and thrive in an environment with low nutrient availability.},\n\tlanguage = {en},\n\tnumber = {7},\n\turldate = {2021-09-08},\n\tjournal = {PLOS ONE},\n\tauthor = {Leuko, Stefan and Koskinen, Kaisa and Sanna, Laura and D’Angeli, Ilenia M. and Waele, Jo De and Marcia, Paolo and Moissl-Eichinger, Christine and Rettberg, Petra},\n\tmonth = jul,\n\tyear = {2017},\n\tkeywords = {Bacteria, Calcite, Caves, Limestone, Manganese, Microbiome, Sediment, Surface water},\n\tpages = {e0180700},\n}\n\n

\n\n\n

\n The bacterial diversity in the Su Bentu Cave in Sardinia was investigated by means of 16S rRNA gene-based analysis. This 15 km long cave, carved in Jurassic limestone, hosts a variety of calcite speleothems, and a long succession of subterranean lakes with mixed granite and carbonate sands. The lower level is occasionally flooded by a rising groundwater level, but with only scarce input of organic remains (leaves and charcoal fragments). On the quiet cave pools there are visible calcite rafts, whereas walls are locally coated with manganese deposits. In the drier upper levels, where organic input is much more subdued, moonmilk—a hydrated calcium-magnesium carbonate speleothem—can be found. Relative humidity approaches 100% and the measured mean annual cave air temperature is 14.8°C. Samples were obtained in 2014 from calcite rafts, moonmilk, manganese oxide deposits and soil (limestone and granite grains). Microclimatic conditions in the cave near the sampling sites, sample properties, physico-chemical parameters of water, and sediment composition were determined. The microbial community of this system is predominately composed of the phyla Proteobacteria, Actinobacteria, Acidobacteria, Nitrospirae, and Firmicutes. Sampling sites near the entrance of the cave and in close proximity of the underground campsite–located 500 meters deep into the cave—revealed the highest diversity as well as the highest number of human associated microorganisms. Two samples obtained in very close proximity of each other near the campsite, indicate that the human impact is localized and is not distributed freely within the system. Analysis of the abundance of bacterial and archaeal amoA genes revealed a far greater abundance of archaeal amoA genes compared to bacterial representatives. The results of this study highlight that human impact is confined to locations that are utilized as campsites and that exploration leaves little microbial trails. Furthermore, we uncovered a highly specialized microbiome, which is perfectly adapted to survive and thrive in an environment with low nutrient availability.\n

\n\n\n

\n \n\n \n \n \n \n \n \n Observational data and orbits of the asteroids discovered at the Molėtai Observatory in 2010-2012.\n \n \n \n \n\n\n \n Włodarczyk, I.; Černis, K.; and Zdanavičius, J.\n\n\n \n\n\n\n Open Astronomy, 26: 35–47. September 2017.\n ADS Bibcode: 2017OAst...26...35W\n\n\n\n
\n\n\n\n \n \n $\"Observational$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{2017OAst...26...35W,\n\ttitle = {Observational data and orbits of the asteroids discovered at the {Molėtai} {Observatory} in 2010-2012},\n\tvolume = {26},\n\turl = {https://ui.adsabs.harvard.edu/abs/2017OAst...26...35W},\n\tdoi = {10.1515/astro-2017-0011},\n\tabstract = {This paper is devoted to the discovery of asteroids at the Molėtai Astronomical Observatory (MAO) in 2010- 2012 together with the orbital analysis of two dynamically interesting Near Earth Objects (NEOs) discovered at the MAO, namely 2006 SF77 and 2010 BT3. We used the OrbFit software v.5.0 to compute orbits and to analyze orbital evolution of 2006 SF77 and 2010 BT3. We computed value of the Lyapunov time: 830 years for 2006 SF77 and 1650 year for 2010 BT3.We also searched for possible impacts of 2006 SF77 and 2010 BT3 with the Earth, Venus and Mars in the next 15000 years.},\n\turldate = {2021-09-08},\n\tjournal = {Open Astronomy},\n\tauthor = {Włodarczyk, Ireneusz and Černis, Kazimieras and Zdanavičius, Justas},\n\tmonth = sep,\n\tyear = {2017},\n\tnote = {ADS Bibcode: 2017OAst...26...35W},\n\tkeywords = {asteroids: search, astrometry, minor planets, orbits},\n\tpages = {35--47},\n}\n\n

\n\n\n\n\n\n

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\n \n\n \n \n \n \n \n \n Genomic Methods and Microbiological Technologies for Profiling Novel and Extreme Environments for the Extreme Microbiome Project (XMP).\n \n \n \n \n\n\n \n Tighe, S.; Afshinnekoo, E.; Rock, T. M.; McGrath, K.; Alexander, N.; McIntyre, A.; Ahsanuddin, S.; Bezdan, D.; Green, S. J.; Joye, S.; Stewart Johnson, S.; Baldwin, D. A.; Bivens, N.; Ajami, N.; Carmical, J. R.; Herriott, I. C.; Colwell, R.; Donia, M.; Foox, J.; Greenfield, N.; Hunter, T.; Hoffman, J.; Hyman, J.; Jorgensen, E.; Krawczyk, D.; Lee, J.; Levy, S.; Garcia-Reyero, N.; Settles, M.; Thomas, K.; Gómez, F.; Schriml, L.; Kyrpides, N.; Zaikova, E.; Penterman, J.; and Mason, C. E.\n\n\n \n\n\n\n Journal of Biomolecular Techniques : JBT, 28(1): 31–39. April 2017.\n \n\n\n\n
\n\n\n\n \n \n $\"Genomic$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{tighe_genomic_2017,\n\ttitle = {Genomic {Methods} and {Microbiological} {Technologies} for {Profiling} {Novel} and {Extreme} {Environments} for the {Extreme} {Microbiome} {Project} ({XMP})},\n\tvolume = {28},\n\tissn = {1524-0215},\n\turl = {https://www.ncbi.nlm.nih.gov/pmc/articles/PMC5345951/},\n\tdoi = {10.7171/jbt.17-2801-004},\n\tabstract = {The Extreme Microbiome Project (XMP) is a project launched by the Association of Biomolecular Resource Facilities Metagenomics Research Group (ABRF MGRG) that focuses on whole genome shotgun sequencing of extreme and unique environments using a wide variety of biomolecular techniques. The goals are multifaceted, including development and refinement of new techniques for the following: 1) the detection and characterization of novel microbes, 2) the evaluation of nucleic acid techniques for extremophilic samples, and 3) the identification and implementation of the appropriate bioinformatics pipelines. Here, we highlight the different ongoing projects that we have been working on, as well as details on the various methods we use to characterize the microbiome and metagenome of these complex samples. In particular, we present data of a novel multienzyme extraction protocol that we developed, called Polyzyme or MetaPolyZyme. Presently, the XMP is characterizing sample sites around the world with the intent of discovering new species, genes, and gene clusters. Once a project site is complete, the resulting data will be publically available. Sites include Lake Hillier in Western Australia, the “Door to Hell” crater in Turkmenistan, deep ocean brine lakes of the Gulf of Mexico, deep ocean sediments from Greenland, permafrost tunnels in Alaska, ancient microbial biofilms from Antarctica, Blue Lagoon Iceland, Ethiopian toxic hot springs, and the acidic hypersaline ponds in Western Australia.},\n\tnumber = {1},\n\turldate = {2021-09-08},\n\tjournal = {Journal of Biomolecular Techniques : JBT},\n\tauthor = {Tighe, Scott and Afshinnekoo, Ebrahim and Rock, Tara M. and McGrath, Ken and Alexander, Noah and McIntyre, Alexa and Ahsanuddin, Sofia and Bezdan, Daniela and Green, Stefan J. and Joye, Samantha and Stewart Johnson, Sarah and Baldwin, Don A. and Bivens, Nathan and Ajami, Nadim and Carmical, Joseph R. and Herriott, Ian Charold and Colwell, Rita and Donia, Mohamed and Foox, Jonathan and Greenfield, Nick and Hunter, Tim and Hoffman, Jessica and Hyman, Joshua and Jorgensen, Ellen and Krawczyk, Diana and Lee, Jodie and Levy, Shawn and Garcia-Reyero, Natàlia and Settles, Matthew and Thomas, Kelley and Gómez, Felipe and Schriml, Lynn and Kyrpides, Nikos and Zaikova, Elena and Penterman, Jon and Mason, Christopher E.},\n\tmonth = apr,\n\tyear = {2017},\n\tpmid = {28337070},\n\tpmcid = {PMC5345951},\n\tpages = {31--39},\n}\n\n

\n\n\n\n\n\n

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\n \n\n \n \n \n \n \n \n Dated eclogitic diamond growth zones reveal variable recycling of crustal carbon through time.\n \n \n \n \n\n\n \n Timmerman, S.; Koornneef, J. M.; Chinn, I. L.; and Davies, G. R.\n\n\n \n\n\n\n Earth and Planetary Science Letters, 463: 178–188. April 2017.\n \n\n\n\n
\n\n\n\n \n \n $\"Dated$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n \n \n \n \n \n \n\n\n\n

@article{timmerman_dated_2017,\n\ttitle = {Dated eclogitic diamond growth zones reveal variable recycling of crustal carbon through time},\n\tvolume = {463},\n\tissn = {0012-821X},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0012821X17300614},\n\tdoi = {10.1016/j.epsl.2017.02.001},\n\tabstract = {Monocrystalline diamonds commonly record complex internal structures reflecting episodic growth linked to changing carbon-bearing fluids in the mantle. Using diamonds to trace the evolution of the deep carbon cycle therefore requires dating of individual diamond growth zones. To this end Rb–Sr and Sm–Nd isotope data are presented from individual eclogitic silicate inclusions from the Orapa and Letlhakane diamond mines, Botswana. δ13C values are reported from the host diamond growth zones. Heterogeneous 87Sr/86Sr ratios (0.7033–0.7097) suggest inclusion formation in multiple and distinct tectono-magmatic environments. Sm–Nd isochron ages were determined based on groups of inclusions with similar trace element chemistry, Sr isotope ratios, and nitrogen aggregation of the host diamond growth zone. Diamond growth events at 0.14±0.09, 0.25±0.04, 1.1±0.09, 1.70±0.34 and 2.33±0.02 Ga can be directly related to regional tectono-magmatic events. Individual diamonds record episodic growth with age differences of up to 2 Ga. Dated diamond zones have variable δ13C values (−5.0 to −33.6‰ vs PDB) and appear to imply changes in subducted material over time. The studied Botswanan diamonds are interpreted to have formed in different tectono-magmatic environments that involve mixing of carbon from three sources that represent: i) subducted biogenic sediments (lightest δ13C, low 87Sr/86Sr); ii) subducted carbonate-rich sediments (heavy δ13C, high 87Sr/86Sr) and iii) depleted upper mantle (heavy δ13C, low 87Sr/86Sr). We infer that older diamonds from these two localities are more likely to have light δ13C due to greater subduction of biogenic sediments that may be related to hotter and more reduced conditions in the Archaean before the Great Oxidation Event at 2.3 Ga. These findings imply a marked temporal change in the nature of subducted carbon beneath Botswana and warrant further study to establish if this is a global phenomenon.},\n\tlanguage = {en},\n\turldate = {2021-09-08},\n\tjournal = {Earth and Planetary Science Letters},\n\tauthor = {Timmerman, S. and Koornneef, J. M. and Chinn, I. L. and Davies, G. R.},\n\tmonth = apr,\n\tyear = {2017},\n\tkeywords = {carbon, dating, diamond, individual silicate inclusions, subduction},\n\tpages = {178--188},\n}\n\n

\n\n\n\n\n\n

\n\n

\n \n 2016\n \n \n (1)\n \n \n

\n \n \n

\n \n\n \n \n \n \n \n \n The thermospheric auroral red line Angle of Linear Polarization.\n \n \n \n \n\n\n \n Lilensten, J.; Barthélemy, M.; Besson, G.; Lamy, H.; Johnsen, M. G.; and Moen, J.\n\n\n \n\n\n\n Journal of Geophysical Research: Space Physics, 121(7): 7125–7134. 2016.\n \n\n\n\n
\n\n\n\n \n \n $\"The$ Paper\n \n \n\n \n \n doi\n \n \n\n \n link\n \n \n\n bibtex\n \n\n \n \n \n abstract \n \n\n \n\n \n \n \n \n \n \n \n\n \n \n \n \n \n \n \n\n\n\n

@article{lilensten_thermospheric_2016,\n\ttitle = {The thermospheric auroral red line {Angle} of {Linear} {Polarization}},\n\tvolume = {121},\n\tissn = {2169-9402},\n\turl = {https://agupubs.onlinelibrary.wiley.com/doi/abs/10.1002/2016JA022941},\n\tdoi = {10.1002/2016JA022941},\n\tabstract = {The auroral red line at 630 nm is linearly polarized. Up to now, only its Degree of Linear Polarization had been studied. In this article, we examine for the first time the Angle of Linear Polarization (AoLP) and we compare the measurements to the apparent angle of the magnetic field at the location of the red line emission. We show that the AoLP is a tracer of the magnetic field configuration. This opens new perspectives, both in the frame of space weather and in the field of planetology.},\n\tlanguage = {en},\n\tnumber = {7},\n\turldate = {2021-09-08},\n\tjournal = {Journal of Geophysical Research: Space Physics},\n\tauthor = {Lilensten, Jean and Barthélemy, Mathieu and Besson, Gérard and Lamy, Hervé and Johnsen, Magnar G. and Moen, Jøran},\n\tyear = {2016},\n\tkeywords = {ionosphere, polarization},\n\tpages = {7125--7134},\n}\n\n

\n\n\n\n\n\n

\n\n

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\n \n\n \n \n \n \n \n Water Ice Particles Sizes on Planetary Surfaces from Infrared Reflectance Spectroscopy: Comparison of Light Scattering Models with Experiments.\n \n \n \n\n\n \n Poch, O.; Ciarniello, M.; Schröder, S.; Kappel, D.; Yoldi, Z.; Jost, B.; Pommerol, A.; Sultana, R.; Beck, P.; Schmitt, B.; Brissaud, O.; Potin, S.; Stephan, K.; and Thomas, N.\n\n\n \n\n\n\n J. Geophys. Res. Planets. .\n \n\n\n\n
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@article{poch_water_nodate,\n\ttitle = {Water {Ice} {Particles} {Sizes} on {Planetary} {Surfaces} from {Infrared} {Reflectance} {Spectroscopy}: {Comparison} of {Light} {Scattering} {Models} with {Experiments}},\n\tjournal = {J. Geophys. Res. Planets},\n\tauthor = {Poch, O. and Ciarniello, M. and Schröder, S. and Kappel, D. and Yoldi, Z. and Jost, B. and Pommerol, A. and Sultana, R. and Beck, P. and Schmitt, B. and Brissaud, O. and Potin, S. and Stephan, K. and Thomas, N.},\n}\n\n

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