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\n \n 2024\n \n \n (1)\n \n \n

\n \n \n

\n \n\n \n \n \n \n \n \n Addendum to “Description, accessibility and usage of SOIR/Venus Express atmospheric profiles of Venus distributed in VESPA (Virtual European Solar and Planetary Access)”.\n \n \n \n \n\n\n \n Trompet, L.; Geunes, Y.; Ooms, T.; Mahieux, A.; Wilquet, V.; Chamberlain, S.; Robert, S.; Thomas, I.; Erard, S.; Cecconi, B.; Le Sidaner, P.; and Vandaele, A.\n\n\n \n\n\n\n Planetary and Space Science, 241: 105842. February 2024.\n \n\n\n\n
\n\n\n\n \n \n $\"Addendum$ 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{trompet_addendum_2024,\n\ttitle = {Addendum to “{Description}, accessibility and usage of {SOIR}/{Venus} {Express} atmospheric profiles of {Venus} distributed in {VESPA} ({Virtual} {European} {Solar} and {Planetary} {Access})”},\n\tvolume = {241},\n\tissn = {00320633},\n\turl = {https://linkinghub.elsevier.com/retrieve/pii/S0032063324000060},\n\tdoi = {10.1016/j.pss.2024.105842},\n\tlanguage = {en},\n\turldate = {2024-05-05},\n\tjournal = {Planetary and Space Science},\n\tauthor = {Trompet, L. and Geunes, Y. and Ooms, T. and Mahieux, A. and Wilquet, V. and Chamberlain, S. and Robert, S. and Thomas, I.R. and Erard, S. and Cecconi, B. and Le Sidaner, P. and Vandaele, A.C.},\n\tmonth = feb,\n\tyear = {2024},\n\tpages = {105842},\n}\n\n

\n\n\n\n

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

\n\n

\n \n 2023\n \n \n (16)\n \n \n

\n \n \n

\n \n\n \n \n \n \n \n \n UCD1+ controlled vocabulary - Updated List of Terms Version 1.5 Version 1.5.\n \n \n \n \n\n\n \n Cecconi, B.; Louys, M.; Preite Martinez, A.; Derrière, S.; Ochsenbein, F.; Erard, S.; and Demleitner, M.\n\n\n \n\n\n\n IVOA Endorsed Note 25 January 2023,125. January 2023.\n ADS Bibcode: 2023ivoa.spec.0125C\n\n\n\n
\n\n\n\n \n \n $\"UCD1+$ 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{cecconi_ucd1_2023,\n\ttitle = {{UCD1}+ controlled vocabulary - {Updated} {List} of {Terms} {Version} 1.5 {Version} 1.5},\n\turl = {https://ui.adsabs.harvard.edu/abs/2023ivoa.spec.0125C},\n\tabstract = {This document describes the list of controlled terms building up the corpus of the Unified Content Descriptors, Version 1+ (UCD1+). The document describing the UCD1+ principles is an IVOA Recommendation (Preite Martinez and Louys et al., 2018), The process to maintain and enrich the UCD list of terms is standardized in (Genova and Louys et al., 2019). It states that successive versions of the UCD1+ vocabulary are distributed in Endorsed Notes within the IVOA. The changes with respect to the version UCDList1.4 have been discussed in the request for modification (RFM) page on (https://wiki.ivoa.net/twiki/bin/view/IVOA/UCDList\\_1-5\\_ RFM) within the IVOA Semantics WG and validated by the UCD science board. Each addition, amendment, etc. is discussed now using VEP-UCD available from the RFM page inspired from the set-up of Vocabulary Enhancement VEP2.0 specification (https://ivoa.net/documents/ Vocabularies/20210525/index.html). VEP-UCD files are referenced from the RFM page and available for further details.},\n\turldate = {2023-12-24},\n\tjournal = {IVOA Endorsed Note 25 January 2023},\n\tauthor = {Cecconi, Baptiste and Louys, Mireille and Preite Martinez, Andrea and Derrière, Sébastien and Ochsenbein, François and Erard, Stéphane and Demleitner, Markus},\n\tmonth = jan,\n\tyear = {2023},\n\tnote = {ADS Bibcode: 2023ivoa.spec.0125C},\n\tpages = {125},\n}\n\n

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

\n\n\n

\n \n\n \n \n \n \n \n \n Virtual European Solar & Planetary Access (VESPA) 2023: Strengthening.\n \n \n \n \n\n\n \n Erard, S.; and VESPA Team\n\n\n \n\n\n\n , 55: 109.03. October 2023.\n Conference Name: AAS/Division for Planetary Sciences Meeting Abstracts ADS Bibcode: 2023DPS....5510903E\n\n\n\n
\n\n\n\n \n \n $\"Virtual$ 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{erard_virtual_2023,\n\ttitle = {Virtual {European} {Solar} \\& {Planetary} {Access} ({VESPA}) 2023: {Strengthening}},\n\tvolume = {55},\n\tshorttitle = {Virtual {European} {Solar} \\& {Planetary} {Access} ({VESPA}) 2023},\n\turl = {https://ui.adsabs.harvard.edu/abs/2023DPS....5510903E},\n\tabstract = {VESPA focuses on adapting Virtual Observatory (VO) techniques to Planetary Science data. The objective is to build a contributory distribution system to easily access and publish data. This activity is held in the EC-funded Europlanet-2024-RI program. Progress during the 3rd year of the program are reported here. Data access. VESPA has defined a specific metadata vocabulary providing uniform description of datasets in the field. In 2022, this EPN-TAP protocol has been approved by the International Virtual Observatory Alliance, and is now the standard to publish Solar System data in the VO. The VESPA portal is a discovery tool to browse the EPN-TAP services. Other access modes are available: scripts, web services, Jupyter notebook, VO tools, etc. Some existing VO tools (TOPCAT, Aladin, CASSIS) are being adapted to these data. Data services. 63 EPN-TAP data services are currently searchable from the VESPA portal. Contributions from space agencies include ESA's PSA, and {\\textasciitilde} 100 datasets from the NASA PDS PPI node (under review). Data infrastructures with EPN-TAP interface (AMDA for planetary plasmas, SSHADE for solid phase spectroscopy, PVOL for amateur images) also develop their content and capacities. Contributions from the community are solicited via an annual call and implementation workshop – one was held in June 2023, and one more workshop is scheduled in the course of the program. Service implementation support and sustainability. A standard workflow to develop and deploy data services has been finalized, relying on a flexible Docker installation of DaCHS and use of a common Gitlab repository (with authentication granted by GÉANT/eduTEAMS). Coming data services. VESPA standards and infrastructure are available to distribute data from the community, in particular to help publicly funded programs fulfill Open Science commitments. A PDS4 dictionary for EPN-TAP is being finalized, which will also provide a data handling and distribution system to nanosat missions. The Europlanet-2024 Research Infrastructure project has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreements No 871149.},\n\turldate = {2023-12-24},\n\tauthor = {Erard, Stéphane and {VESPA Team}},\n\tmonth = oct,\n\tyear = {2023},\n\tnote = {Conference Name: AAS/Division for Planetary Sciences Meeting Abstracts\nADS Bibcode: 2023DPS....5510903E},\n\tpages = {109.03},\n}\n\n

\n\n\n

\n VESPA focuses on adapting Virtual Observatory (VO) techniques to Planetary Science data. The objective is to build a contributory distribution system to easily access and publish data. This activity is held in the EC-funded Europlanet-2024-RI program. Progress during the 3rd year of the program are reported here. Data access. VESPA has defined a specific metadata vocabulary providing uniform description of datasets in the field. In 2022, this EPN-TAP protocol has been approved by the International Virtual Observatory Alliance, and is now the standard to publish Solar System data in the VO. The VESPA portal is a discovery tool to browse the EPN-TAP services. Other access modes are available: scripts, web services, Jupyter notebook, VO tools, etc. Some existing VO tools (TOPCAT, Aladin, CASSIS) are being adapted to these data. Data services. 63 EPN-TAP data services are currently searchable from the VESPA portal. Contributions from space agencies include ESA's PSA, and ~ 100 datasets from the NASA PDS PPI node (under review). Data infrastructures with EPN-TAP interface (AMDA for planetary plasmas, SSHADE for solid phase spectroscopy, PVOL for amateur images) also develop their content and capacities. Contributions from the community are solicited via an annual call and implementation workshop – one was held in June 2023, and one more workshop is scheduled in the course of the program. Service implementation support and sustainability. A standard workflow to develop and deploy data services has been finalized, relying on a flexible Docker installation of DaCHS and use of a common Gitlab repository (with authentication granted by GÉANT/eduTEAMS). Coming data services. VESPA standards and infrastructure are available to distribute data from the community, in particular to help publicly funded programs fulfill Open Science commitments. A PDS4 dictionary for EPN-TAP is being finalized, which will also provide a data handling and distribution system to nanosat missions. The Europlanet-2024 Research Infrastructure project has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreements No 871149.\n

\n\n\n

\n \n\n \n \n \n \n \n \n Discovery portal in planetary science using Vespa.\n \n \n \n \n\n\n \n Le Sidaner, P.; Cecconi, B.; Erard, S.; Chauvin, C.; and azria , c.\n\n\n \n\n\n\n , 55: 117.02. October 2023.\n Conference Name: AAS/Division for Planetary Sciences Meeting Abstracts ADS Bibcode: 2023DPS....5511702L\n\n\n\n
\n\n\n\n \n \n $\"Discovery$ 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{le_sidaner_discovery_2023,\n\ttitle = {Discovery portal in planetary science using {Vespa}},\n\tvolume = {55},\n\turl = {https://ui.adsabs.harvard.edu/abs/2023DPS....5511702L},\n\tabstract = {espa is a Europlanet-funded project that was conceived during the FP6 programme, developed during the H2020 programme and constantly improved during the Europlanet-2024 Research Infrastructure programme. Vespa aims to organise the dissemination of solar system data using the infrastructure and tools of the International Virtual Observatory alliance (IVOA). The Vespa project has been one of the pillars of planetary science's involvement in the IVOA. The data model is now accepted as a standard and EPN-TAP services are accessible from the registry. One of Vespa's major challenges is to provide access to the diversity of planetary science data. The data is accessible in a free and standard way. A simple way of finding data is to search via a portal https://vespa.obspm.fr. In parallel with this portal, which interrogates an eco system of distributed data, we are developing a data discovery portal providing an intuitive view of the content of nearly 200 data services, including the PSA and NASA's PPI node. I propose to present the data discovery portal and the interaction with the classic search portal Vespa.},\n\turldate = {2023-12-24},\n\tauthor = {Le Sidaner, Pierre and Cecconi, Baptiste and Erard, Stéphane and Chauvin, Cyril and azria, chloe},\n\tmonth = oct,\n\tyear = {2023},\n\tnote = {Conference Name: AAS/Division for Planetary Sciences Meeting Abstracts\nADS Bibcode: 2023DPS....5511702L},\n\tpages = {117.02},\n}\n\n

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

\n\n\n

\n \n\n \n \n \n \n \n \n Drift rates of major Neptunian features between 2018 and 2021.\n \n \n \n \n\n\n \n Chavez, E.; Redwing, E.; De Pater, I.; Hueso, R.; Molter, E. M.; Wong, M. H.; Alvarez, C.; Gates, E.; De Kleer, K.; Aycock, J.; Mcilroy, J.; Pelletier, J.; Ridenour, A.; Sánchez-Lavega, A.; Rojas, J. F.; and Stickel, T.\n\n\n \n\n\n\n Icarus, 401: 115604. September 2023.\n \n\n\n\n
\n\n\n\n \n \n $\"Drift$ 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{chavez_drift_2023,\n\ttitle = {Drift rates of major {Neptunian} features between 2018 and 2021},\n\tvolume = {401},\n\tissn = {00191035},\n\turl = {https://linkinghub.elsevier.com/retrieve/pii/S0019103523001811},\n\tdoi = {10.1016/j.icarus.2023.115604},\n\tlanguage = {en},\n\turldate = {2023-12-21},\n\tjournal = {Icarus},\n\tauthor = {Chavez, Erandi and Redwing, Erin and De Pater, Imke and Hueso, Ricardo and Molter, Edward M. and Wong, Michael H. and Alvarez, Carlos and Gates, Elinor and De Kleer, Katherine and Aycock, Joel and Mcilroy, Jason and Pelletier, John and Ridenour, Anthony and Sánchez-Lavega, Agustín and Rojas, Jose Félix and Stickel, Terry},\n\tmonth = sep,\n\tyear = {2023},\n\tpages = {115604},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Venus cloud discontinuity in 2022: The first long-term study with uninterrupted observations.\n \n \n \n \n\n\n \n Peralta, J.; Cidadão, A.; Morrone, L.; Foster, C.; Bullock, M.; Young, E. F.; Garate-Lopez, I.; Sánchez-Lavega, A.; Horinouchi, T.; Imamura, T.; Kardasis, E.; Yamazaki, A.; and Watanabe, S.\n\n\n \n\n\n\n Astronomy & Astrophysics, 672: L2. April 2023.\n \n\n\n\n
\n\n\n\n \n \n $\"Venus$ 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{peralta_venus_2023,\n\ttitle = {Venus cloud discontinuity in 2022: {The} first long-term study with uninterrupted observations},\n\tvolume = {672},\n\tissn = {0004-6361, 1432-0746},\n\tshorttitle = {Venus cloud discontinuity in 2022},\n\turl = {https://www.aanda.org/10.1051/0004-6361/202244822},\n\tdoi = {10.1051/0004-6361/202244822},\n\tabstract = {Context.\n              First identified in 2016 by the Japan Aerospace eXploration Agency (JAXA) Akatsuki mission, the discontinuity or disruption is a recurrent wave observed to propagate over decades at the deeper clouds of Venus (47–56 km above the surface), while its absence at the top of the clouds (∼70 km) suggests that it dissipates at the upper clouds and contributes to the maintenance of the puzzling atmospheric superrotation of Venus through wave-mean flow interaction.\n            \n            \n              Aims.\n              Taking advantage of the campaign of ground-based observations undertaken in coordination with the Akatsuki mission from December 2021 until July 2022, we undertook the longest uninterrupted monitoring of the cloud discontinuity to date to obtain a pioneering long-term characterisation of its main properties and to better constrain its recurrence and lifetime.\n            \n            \n              Methods.\n              The dayside upper, middle, and nightside lower clouds were studied with images acquired by the Akatsuki Ultraviolet Imager (UVI), amateur observers, and SpeX at the NASA Infrared Telescope Facility (IRTF). Hundreds of images were inspected in search of the discontinuity events and to measure key properties such as its dimensions, orientation, and rotation period.\n            \n            \n              Results.\n              We succeeded in tracking the discontinuity at the middle clouds during 109 days without interruption. The discontinuity exhibited properties nearly identical to measurements in 2016 and 2020, with an orientation of 91° ±8°, length of 4100 ± 800 km, width of 500 ± 100 km, and a rotation period of 5.11 ± 0.09 days. Ultraviolet images during 13–14 June 2022 suggest that the discontinuity may have manifested at the top of the clouds during ∼21 h as a result of an altitude change in the critical level for this wave, due to slower zonal winds.},\n\turldate = {2023-12-21},\n\tjournal = {Astronomy \\& Astrophysics},\n\tauthor = {Peralta, J. and Cidadão, A. and Morrone, L. and Foster, C. and Bullock, M. and Young, E. F. and Garate-Lopez, I. and Sánchez-Lavega, A. and Horinouchi, T. and Imamura, T. and Kardasis, E. and Yamazaki, A. and Watanabe, S.},\n\tmonth = apr,\n\tyear = {2023},\n\tpages = {L2},\n}\n\n

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

\n\n\n

\n \n\n \n \n \n \n \n \n IVOA Note - Using Wikidata for an Observation Facility Vocabulary.\n \n \n \n \n\n\n \n Cecconi; Debisschop; Louys; Perret; and Demleitner\n\n\n \n\n\n\n Technical Report November 2023.\n \n\n\n\n
\n\n\n\n \n \n $\"IVOA$ 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

@techreport{cecconi_ivoa_2023,\n\ttitle = {{IVOA} {Note} - {Using} {Wikidata} for an {Observation} {Facility} {Vocabulary}},\n\turl = {https://ivoa.net/documents/Notes/ObsFacilityWikidata/index.html},\n\turldate = {2023-12-19},\n\tauthor = {{Cecconi} and {Debisschop} and {Louys} and {Perret} and {Demleitner}},\n\tmonth = nov,\n\tyear = {2023},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Carbon Dioxide Retrievals From NOMAD‐SO on ESA's ExoMars Trace Gas Orbiter and Temperature Profile Retrievals With the Hydrostatic Equilibrium Equation: 2. Temperature Variabilities in the Mesosphere at Mars Terminator.\n \n \n \n \n\n\n \n Trompet, L.; Vandaele, A. C.; Thomas, I.; Aoki, S.; Daerden, F.; Erwin, J.; Flimon, Z.; Mahieux, A.; Neary, L.; Robert, S.; Villanueva, G.; Liuzzi, G.; López‐Valverde, M. A.; Brines, A.; Bellucci, G.; Lopez‐Moreno, J. J.; and Patel, M. R.\n\n\n \n\n\n\n Journal of Geophysical Research: Planets, 128(3): e2022JE007279. March 2023.\n \n\n\n\n
\n\n\n\n \n \n $\"Carbon$ 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{trompet_carbon_2023,\n\ttitle = {Carbon {Dioxide} {Retrievals} {From} {NOMAD}‐{SO} on {ESA}'s {ExoMars} {Trace} {Gas} {Orbiter} and {Temperature} {Profile} {Retrievals} {With} the {Hydrostatic} {Equilibrium} {Equation}: 2. {Temperature} {Variabilities} in the {Mesosphere} at {Mars} {Terminator}},\n\tvolume = {128},\n\tissn = {2169-9097, 2169-9100},\n\tshorttitle = {Carbon {Dioxide} {Retrievals} {From} {NOMAD}‐{SO} on {ESA}'s {ExoMars} {Trace} {Gas} {Orbiter} and {Temperature} {Profile} {Retrievals} {With} the {Hydrostatic} {Equilibrium} {Equation}},\n\turl = {https://agupubs.onlinelibrary.wiley.com/doi/10.1029/2022JE007279},\n\tdoi = {10.1029/2022JE007279},\n\tlanguage = {en},\n\tnumber = {3},\n\turldate = {2023-04-23},\n\tjournal = {Journal of Geophysical Research: Planets},\n\tauthor = {Trompet, L. and Vandaele, A. C. and Thomas, I. and Aoki, S. and Daerden, F. and Erwin, J. and Flimon, Z. and Mahieux, A. and Neary, L. and Robert, S. and Villanueva, G. and Liuzzi, G. and López‐Valverde, M. A. and Brines, A. and Bellucci, G. and Lopez‐Moreno, J. J. and Patel, M. R.},\n\tmonth = mar,\n\tyear = {2023},\n\tpages = {e2022JE007279},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Carbon Dioxide Retrievals From NOMAD‐SO on ESA's ExoMars Trace Gas Orbiter and Temperature Profiles Retrievals With the Hydrostatic Equilibrium Equation: 1. Description of the Method.\n \n \n \n \n\n\n \n Trompet, L.; Vandaele, A. C.; Thomas, I.; Aoki, S.; Daerden, F.; Erwin, J.; Flimon, Z.; Mahieux, A.; Neary, L.; Robert, S.; Villanueva, G.; Liuzzi, G.; López‐Valverde, M. A.; Brines, A.; Bellucci, G.; López‐Moreno, J. J.; and Patel, M. R.\n\n\n \n\n\n\n Journal of Geophysical Research: Planets, 128(3): e2022JE007277. March 2023.\n \n\n\n\n
\n\n\n\n \n \n $\"Carbon$ 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{trompet_carbon_2023-1,\n\ttitle = {Carbon {Dioxide} {Retrievals} {From} {NOMAD}‐{SO} on {ESA}'s {ExoMars} {Trace} {Gas} {Orbiter} and {Temperature} {Profiles} {Retrievals} {With} the {Hydrostatic} {Equilibrium} {Equation}: 1. {Description} of the {Method}},\n\tvolume = {128},\n\tissn = {2169-9097, 2169-9100},\n\tshorttitle = {Carbon {Dioxide} {Retrievals} {From} {NOMAD}‐{SO} on {ESA}'s {ExoMars} {Trace} {Gas} {Orbiter} and {Temperature} {Profiles} {Retrievals} {With} the {Hydrostatic} {Equilibrium} {Equation}},\n\turl = {https://agupubs.onlinelibrary.wiley.com/doi/10.1029/2022JE007277},\n\tdoi = {10.1029/2022JE007277},\n\tlanguage = {en},\n\tnumber = {3},\n\turldate = {2023-04-23},\n\tjournal = {Journal of Geophysical Research: Planets},\n\tauthor = {Trompet, L. and Vandaele, A. C. and Thomas, I. and Aoki, S. and Daerden, F. and Erwin, J. and Flimon, Z. and Mahieux, A. and Neary, L. and Robert, S. and Villanueva, G. and Liuzzi, G. and López‐Valverde, M. A. and Brines, A. and Bellucci, G. and López‐Moreno, J. J. and Patel, M. R.},\n\tmonth = mar,\n\tyear = {2023},\n\tpages = {e2022JE007277},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n EPN-TAP: the VO standard to share and access Solar System data.\n \n \n \n \n\n\n \n Erard, S.; Cecconi, B.; Le Sidaner, P.; Demleitner, M.; and Taylor, M.\n\n\n \n\n\n\n . December 2023.\n Publisher: Zenodo\n\n\n\n
\n\n\n\n \n \n $\"EPN-TAP:$ 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{erard_epn-tap_2023,\n\ttitle = {{EPN}-{TAP}: the {VO} standard to share and access {Solar} {System} data},\n\tcopyright = {Creative Commons Attribution 4.0 International},\n\tshorttitle = {{EPN}-{TAP}},\n\turl = {https://zenodo.org/doi/10.5281/zenodo.10255586},\n\tdoi = {10.5281/ZENODO.10255586},\n\tabstract = {A new protocol has been adopted in the Virtual Ob- servatory to share and access data related to the Solar System in the broadest sense. This relies on the Table Access Protocol (TAP) standard and a specific vocab- ulary called EPNCore used to describe quantities of interest for Planetary Science, heliophysics, exoplan- ets, and related laboratory measurements. It is de- scribed here, together with possible usages beyond the basic access to public databases.},\n\turldate = {2023-12-07},\n\tauthor = {Erard, Stéphane and Cecconi, Baptiste and Le Sidaner, Pierre and Demleitner, Markus and Taylor, Mark},\n\tmonth = dec,\n\tyear = {2023},\n\tnote = {Publisher: Zenodo},\n}\n\n

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\n \n\n \n \n \n \n \n \n Formulation of spectral indexes from M3 cubes for lunar mineral exploration using python.\n \n \n \n \n\n\n \n Valencia, J. E. S.; Rosi, A. P.; and Nodjourmi, G.\n\n\n \n\n\n\n Technical Report Copernicus Meetings, 2023.\n \n\n\n\n
\n\n\n\n \n \n $\"Formulation$ 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

@techreport{valencia_formulation_2023,\n\ttitle = {Formulation of spectral indexes from {M3} cubes for lunar mineral exploration using python},\n\turl = {https://meetingorganizer.copernicus.org/EGU23/EGU23-8161.html?pdf},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Valencia, Javier Eduardo Suarez and Rosi, Angelo Pio and Nodjourmi, Giacomo},\n\tyear = {2023},\n}\n\n

\n\n\n\n

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\n \n\n \n \n \n \n \n \n Sublimation-driven formation of recent mass flows on Mars: experimental tests in low-pressure environments.\n \n \n \n \n\n\n \n Haas, T. d.; Roelofs, L.; Conway, S.; McElwaine, J.; Merrison, J.; Patel, M.; and Sylvest, M.\n\n\n \n\n\n\n Technical Report EGU23-1451, Copernicus Meetings, February 2023.\n \n\n\n\n
\n\n\n\n \n \n $\"Sublimation-driven$ 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

@techreport{haas_sublimation-driven_2023,\n\ttitle = {Sublimation-driven formation of recent mass flows on {Mars}: experimental tests in low-pressure environments},\n\tshorttitle = {Sublimation-driven formation of recent mass flows on {Mars}},\n\turl = {https://meetingorganizer.copernicus.org/EGU23/EGU23-1451.html},\n\tlanguage = {en},\n\tnumber = {EGU23-1451},\n\turldate = {2023-06-26},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Haas, Tjalling de and Roelofs, Lonneke and Conway, Susan and McElwaine, Jim and Merrison, Jon and Patel, Manish and Sylvest, Matthew},\n\tmonth = feb,\n\tyear = {2023},\n\tdoi = {10.5194/egusphere-egu23-1451},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n CO2-driven granular flows as erosional forces on present-day Mars.\n \n \n \n \n\n\n \n Roelofs, L.; Merrison, J.; Conway, S.; and Haas, T. d.\n\n\n \n\n\n\n Technical Report EGU23-2626, Copernicus Meetings, February 2023.\n \n\n\n\n
\n\n\n\n \n \n $\"CO2-driven$ 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

@techreport{roelofs_co2-driven_2023,\n\ttitle = {{CO2}-driven granular flows as erosional forces on present-day {Mars}},\n\turl = {https://meetingorganizer.copernicus.org/EGU23/EGU23-2626.html},\n\tlanguage = {en},\n\tnumber = {EGU23-2626},\n\turldate = {2023-06-26},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Roelofs, Lonneke and Merrison, Jonathan and Conway, Susan and Haas, Tjallng de},\n\tmonth = feb,\n\tyear = {2023},\n\tdoi = {10.5194/egusphere-egu23-2626},\n}\n\n

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\n \n\n \n \n \n \n \n \n Hydrothermal Alteration of Ultramafic Rocks in Ladon Basin, Mars—Insights From CaSSIS, HiRISE, CRISM, and CTX.\n \n \n \n \n\n\n \n Mège, D.; Gurgurewicz, J.; Massironi, M.; Pozzobon, R.; Tognon, G.; Pajola, M.; Tornabene, L. L.; Lucchetti, A.; Baschetti, B.; Davis, J. M.; Hauber, E.; De Toffoli, B.; Douté, S.; Keszthelyi, L.; Marinangeli, L.; Perry, J.; Pommerol, A.; Pompilio, L.; Rossi, A. P.; Seelos, F.; Sauro, F.; Ziethe, R.; Cremonese, G.; and Thomas, N.\n\n\n \n\n\n\n Journal of Geophysical Research: Planets, 128(1): e2022JE007223. 2023.\n _eprint: https://onlinelibrary.wiley.com/doi/pdf/10.1029/2022JE007223\n\n\n\n
\n\n\n\n \n \n $\"Hydrothermal$ 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{mege_hydrothermal_2023,\n\ttitle = {Hydrothermal {Alteration} of {Ultramafic} {Rocks} in {Ladon} {Basin}, {Mars}—{Insights} {From} {CaSSIS}, {HiRISE}, {CRISM}, and {CTX}},\n\tvolume = {128},\n\tissn = {2169-9100},\n\turl = {https://onlinelibrary.wiley.com/doi/abs/10.1029/2022JE007223},\n\tdoi = {10.1029/2022JE007223},\n\tabstract = {The evolution of the Ladon basin has been marked by intense geological activity and the discharge of huge volumes of water from the Martian highlands to the lowlands in the late Noachian and Hesperian. We explore the potential of the ExoMars Trace Gas Orbiter/Color and Stereo Surface Imaging System color image data set for geological interpretation and show that it is particularly effective for geologic mapping in combination with other data sets such as HiRISE, Context, and Compact Reconnaissance Imaging Spectrometer for Mars. The study area displays dark lobate flows of upper Hesperian to early Amazonian age, which were likely extruded from a regional extensional fault network. Spectral analysis suggests that these flows and the underlying rocks are ultramafic. Two distinct altered levels are observed below the lobate flows. The upper, yellow-orange level shows hundreds of structurally controlled narrow ridges reminiscent of ridges of listwanite, a suite of silicified, fracture-controlled silica-carbonate rocks derived from an ultramafic source and from serpentine. In addition to serpentinite, the detected mineral assemblages may include chlorite, carbonates, and talc. Kaolin minerals are detected in the lower, white level, which could have formed by groundwater alteration of plagioclase in the volcanic pile. Volcanism, tectonics, hydrothermal activity, and kaolinization are interpreted to be coeval, with hydrothermal activity and kaolinization controlled by the interactions between the aquifer and the hot, ultramafic lobate flows. Following our interpretations, East Ladon may host the first listwanite ridges described on Mars, involving a hydrothermal system rooted in a Hesperian aquifer and affecting ultramafic rocks from a magmatic source yet to be identified.},\n\tlanguage = {en},\n\tnumber = {1},\n\turldate = {2023-05-12},\n\tjournal = {Journal of Geophysical Research: Planets},\n\tauthor = {Mège, Daniel and Gurgurewicz, Joanna and Massironi, Matteo and Pozzobon, Riccardo and Tognon, Gloria and Pajola, Maurizio and Tornabene, Livio L. and Lucchetti, Alice and Baschetti, Beatrice and Davis, Joel M. and Hauber, Ernst and De Toffoli, Barbara and Douté, Sylvain and Keszthelyi, Laszlo and Marinangeli, Lucia and Perry, Jason and Pommerol, Antoine and Pompilio, Loredana and Rossi, Angelo Pio and Seelos, Frank and Sauro, Francesco and Ziethe, Ruth and Cremonese, Gabriele and Thomas, Nicolas},\n\tyear = {2023},\n\tnote = {\\_eprint: https://onlinelibrary.wiley.com/doi/pdf/10.1029/2022JE007223},\n\tkeywords = {CaSSIS, ExoMars, Ladon, Mars, listwanite, serpentine},\n\tpages = {e2022JE007223},\n}\n\n

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\n \n\n \n \n \n \n \n \n Solid−gas carbonate formation during dust events on Mars.\n \n \n \n \n\n\n \n Mao, W.; Fu, X.; Wu, Z.; Zhang, J.; Ling, Z.; Liu, Y.; Zhao, Y. S.; Changela, H. G; Ni, Y.; Yan, F.; and Zou, Y.\n\n\n \n\n\n\n National Science Review, 10(4): nwac293. March 2023.\n \n\n\n\n
\n\n\n\n \n \n $\"Solid−gas$ 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{mao_solidgas_2023,\n\ttitle = {Solid−gas carbonate formation during dust events on {Mars}},\n\tvolume = {10},\n\tissn = {2095-5138, 2053-714X},\n\turl = {https://academic.oup.com/nsr/article/doi/10.1093/nsr/nwac293/6985011},\n\tdoi = {10.1093/nsr/nwac293},\n\tabstract = {Electrostatic discharge experiments under simulated martian atmospheric conditions indicate that atmospheric CO2 has been sequestered into carbonate by the Mars dust activities during the Amazonia era.},\n\tlanguage = {en},\n\tnumber = {4},\n\turldate = {2023-04-24},\n\tjournal = {National Science Review},\n\tauthor = {Mao, Wenshuo and Fu, Xiaohui and Wu, Zhongchen and Zhang, Jiang and Ling, Zongcheng and Liu, Yang and Zhao, Yu-Yan Sara and Changela, Hitesh G and Ni, Yuheng and Yan, Fabao and Zou, Yongliao},\n\tmonth = mar,\n\tyear = {2023},\n\tpages = {nwac293},\n}\n\n

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\n \n\n \n \n \n \n \n Multidisciplinary analysis of pit craters at Hale Crater, Mars.\n \n \n \n\n\n \n Mantegazza, M.; Spagnuolo, M. G; and Rossi, A. P\n\n\n \n\n\n\n Icarus,115495. 2023.\n Publisher: Elsevier\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

@article{mantegazza_multidisciplinary_2023,\n\ttitle = {Multidisciplinary analysis of pit craters at {Hale} {Crater}, {Mars}},\n\tissn = {0019-1035},\n\tjournal = {Icarus},\n\tauthor = {Mantegazza, Mara and Spagnuolo, Mauro G and Rossi, Angelo P},\n\tyear = {2023},\n\tnote = {Publisher: Elsevier},\n\tpages = {115495},\n}\n\n

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\n \n\n \n \n \n \n \n \n Time-frequency catalogue: JSON implementation and python library.\n \n \n \n \n\n\n \n Cecconi, B.; Louis, C. K.; Bonnin, X.; Loh, A.; and Taylor, M. B.\n\n\n \n\n\n\n Frontiers in Astronomy and Space Sciences, 9. 2023.\n \n\n\n\n
\n\n\n\n \n \n $\"Time-frequency$ 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{cecconi_time-frequency_2023,\n\ttitle = {Time-frequency catalogue: {JSON} implementation and python library},\n\tvolume = {9},\n\tissn = {2296-987X},\n\tshorttitle = {Time-frequency catalogue},\n\turl = {https://www.frontiersin.org/articles/10.3389/fspas.2022.1049677},\n\tabstract = {TFCat (Time-Frequency Catalogue) is a data interchange format based on JSON (JavaScript Object Notation), which has been initially designed for exchanging low frequency radio events and features. It defines several types of JSON objects and how they are combined to represent data related to temporal-spectral features of a time spectrogram (a.k.a., dynamic spectrum), their properties, and their temporal and spectral extents. This implementation is inheriting from the GeoJSON file format. The TFCat python library is implementing this specification and provides a software interface permitting to create, update and validate TFCat objects efficiently.},\n\turldate = {2023-03-06},\n\tjournal = {Frontiers in Astronomy and Space Sciences},\n\tauthor = {Cecconi, Baptiste and Louis, Corentin K. and Bonnin, Xavier and Loh, Alan and Taylor, Mark B.},\n\tyear = {2023},\n}\n\n

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

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\n \n 2022\n \n \n (42)\n \n \n

\n \n \n

\n \n\n \n \n \n \n \n \n Approach towards a Holistic Management of Research Data in Planetary Science—Use Case Study Based on Remote Sensing Data.\n \n \n \n \n\n\n \n Nass, A.; Mühlbauer, M.; Heinen, T.; Böck, M.; Munteanu, R.; D’Amore, M.; Riedlinger, T.; Roatsch, T.; Strunz, G.; and Helbert, J.\n\n\n \n\n\n\n Remote Sensing, 14(7): 1598. March 2022.\n \n\n\n\n
\n\n\n\n \n \n $\"Approach$ 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{nass_approach_2022,\n\ttitle = {Approach towards a {Holistic} {Management} of {Research} {Data} in {Planetary} {Science}—{Use} {Case} {Study} {Based} on {Remote} {Sensing} {Data}},\n\tvolume = {14},\n\tcopyright = {https://creativecommons.org/licenses/by/4.0/},\n\tissn = {2072-4292},\n\turl = {https://www.mdpi.com/2072-4292/14/7/1598},\n\tdoi = {10.3390/rs14071598},\n\tabstract = {In the planetary sciences, the volume of remote sensing data and derived research products has been continuously increasing over the last five decades. The amount and complexity of data require growing sophistication in data analysis, data management, and data provision targeted at a growing research community. In order to efficiently manage and facilitate the reuse of research data and to provide stable and long-term access, sustainable research data solutions are needed. We here present a prototype for structured storage, management, and visualisation of planetary research data and discuss the particular benefits, as well as challenges of such an information system for data management, for establishing data references by cross-linking information, and for improving the visibility of data products. The prototype is a co-development of two research institutes of the German Aerospace Center (DLR) and is based on two components: the Earth Observation Center (EOC) Geoservice, which constitutes an infrastructure providing data storage and management capabilities, as well as an interface compliant with collaborative and web-based data access services, and the Environmental and Crisis Information Systems (UKIS), a framework for the implementation of geoscientific web applications.},\n\tlanguage = {en},\n\tnumber = {7},\n\turldate = {2024-05-08},\n\tjournal = {Remote Sensing},\n\tauthor = {Nass, Andrea and Mühlbauer, Martin and Heinen, Torsten and Böck, Mathias and Munteanu, Robert and D’Amore, Mario and Riedlinger, Torsten and Roatsch, Thomas and Strunz, Günter and Helbert, Jörn},\n\tmonth = mar,\n\tyear = {2022},\n\tpages = {1598},\n}\n\n

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\n \n\n \n \n \n \n \n \n Mercury exploration with MATISSE tool.\n \n \n \n \n\n\n \n Rognini, E.; Camplone, V.; Zinzi, A.; Mura, A.; Milillo, A.; Massironi, M.; Rossi, A. P.; Zucca, F.; and Capria, M. T.\n\n\n \n\n\n\n Technical Report Copernicus Meetings, 2022.\n \n\n\n\n
\n\n\n\n \n \n $\"Mercury$ 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

@techreport{rognini_mercury_2022,\n\ttitle = {Mercury exploration with {MATISSE} tool},\n\turl = {https://www.europlanet-society.org/wp-content/uploads/2024/02/375.pdf},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Rognini, Edoardo and Camplone, Veronica and Zinzi, Angelo and Mura, Alessandro and Milillo, Anna and Massironi, Matteo and Rossi, Angelo Pio and Zucca, Francesco and Capria, Maria Teresa},\n\tyear = {2022},\n}\n\n

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\n \n\n \n \n \n \n \n \n EXPLORE Lunar Scientific Data Applications: L-Explo and L-Hex.\n \n \n \n \n\n\n \n Nodjoumi, G.; Valencia, J. E.; Brandt, C.; Cox, N. L.; and Rossi, A. P\n\n\n \n\n\n\n In pages EPSC2022–966, 2022. \n \n\n\n\n
\n\n\n\n \n \n $\"EXPLORE$ 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

@inproceedings{nodjoumi_explore_2022,\n\ttitle = {{EXPLORE} {Lunar} {Scientific} {Data} {Applications}: {L}-{Explo} and {L}-{Hex}},\n\turl = {https://www.europlanet-society.org/wp-content/uploads/2024/02/372.pdf},\n\tauthor = {Nodjoumi, Giacomo and Valencia, Javier ES and Brandt, Carlos and Cox, Nick LJ and Rossi, Angelo P},\n\tyear = {2022},\n\tpages = {EPSC2022--966},\n}\n\n

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\n \n\n \n \n \n \n \n \n GEM-Mars GCM products and tools available through the VESPA portal.\n \n \n \n \n\n\n \n Trompet, L.; Daerden, F.; Neary, L.; Erwin, J.; Vandaele, A. C.; and Erard, S.\n\n\n \n\n\n\n Technical Report EPSC2022-4, Copernicus Meetings, July 2022.\n Conference Name: EPSC2022\n\n\n\n
\n\n\n\n \n \n $\"GEM-Mars$ 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

@techreport{trompet_gem-mars_2022,\n\ttitle = {{GEM}-{Mars} {GCM} products and tools available through the {VESPA} portal.},\n\turl = {https://www.europlanet-society.org/wp-content/uploads/2024/02/284.pdf},\n\tlanguage = {en},\n\tnumber = {EPSC2022-4},\n\turldate = {2023-01-02},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Trompet, Loïc and Daerden, Frank and Neary, Lori and Erwin, Justin and Vandaele, Ann Carine and Erard, Stéphane},\n\tmonth = jul,\n\tyear = {2022},\n\tdoi = {10.5194/epsc2022-4},\n\tnote = {Conference Name: EPSC2022},\n}\n\n

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\n \n\n \n \n \n \n \n \n The Future and Sustainability of Transnational Access in Europlanet Research Infrastructure.\n \n \n \n \n\n\n \n Davies, G.; Westrenen, W. v.; Merrison, J.; Russell, S.; Cavalazzi, B.; L'Haridon, J.; and Mason, N.\n\n\n \n\n\n\n Technical Report EPSC2022-126, Copernicus Meetings, July 2022.\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

@techreport{davies_future_2022,\n\ttitle = {The {Future} and {Sustainability} of {Transnational} {Access} in {Europlanet} {Research} {Infrastructure}},\n\turl = {https://www.europlanet-society.org/wp-content/uploads/2024/02/228-1.pdf},\n\tlanguage = {en},\n\tnumber = {EPSC2022-126},\n\turldate = {2022-11-30},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Davies, Gareth and Westrenen, Wim van and Merrison, Jonathan and Russell, Sara and Cavalazzi, Barbara and L'Haridon, Jonas and Mason, Nigel},\n\tmonth = jul,\n\tyear = {2022},\n\tdoi = {10.5194/epsc2022-126},\n}\n\n

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\n \n\n \n \n \n \n \n \n The Europlanet Early Career (EPEC) Network: Building a Community to Support Junior Researchers.\n \n \n \n \n\n\n \n Luzzi, E.; Belgacem, I.; and Mirino, M.\n\n\n \n\n\n\n Technical Report EPSC2022-586, Copernicus Meetings, July 2022.\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

@techreport{luzzi_europlanet_2022,\n\ttitle = {The {Europlanet} {Early} {Career} ({EPEC}) {Network}: {Building} a {Community} to {Support} {Junior} {Researchers}},\n\tshorttitle = {The {Europlanet} {Early} {Career} ({EPEC}) {Network}},\n\turl = {https://www.europlanet-society.org/wp-content/uploads/2024/02/229-1.pdf},\n\tlanguage = {en},\n\tnumber = {EPSC2022-586},\n\turldate = {2022-11-30},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Luzzi, Erica and Belgacem, Ines and Mirino, Melissa},\n\tmonth = jul,\n\tyear = {2022},\n\tdoi = {10.5194/epsc2022-586},\n}\n\n

\n\n\n\n

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\n \n\n \n \n \n \n \n \n MOMSTER, a Europlanet-funded STEAM education project.\n \n \n \n \n\n\n \n Calders, S.; Lamy, H.; Sterken, M.; Lefever, K.; Kolenberg, K.; Anciaux, M.; and Coeckelberghs, H.\n\n\n \n\n\n\n Technical Report EPSC2022-443, Copernicus Meetings, July 2022.\n \n\n\n\n
\n\n\n\n \n \n $\"MOMSTER,$ 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

@techreport{calders_momster_2022,\n\ttitle = {{MOMSTER}, a {Europlanet}-funded {STEAM} education project},\n\turl = {https://www.europlanet-society.org/wp-content/uploads/2024/02/230-1.pdf},\n\tlanguage = {en},\n\tnumber = {EPSC2022-443},\n\turldate = {2022-11-30},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Calders, Stijn and Lamy, Hervé and Sterken, Mieke and Lefever, Karolien and Kolenberg, Katrien and Anciaux, Michel and Coeckelberghs, Hans},\n\tmonth = jul,\n\tyear = {2022},\n\tdoi = {10.5194/epsc2022-443},\n}\n\n

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\n \n\n \n \n \n \n \n \n Supporting Open Science with the Europlanet Research Infrastructure.\n \n \n \n \n\n\n \n Heward, A.; and DeWitt, J.\n\n\n \n\n\n\n In July 2022. Copernicus Meetings\n \n\n\n\n
\n\n\n\n \n \n $\"Supporting$ 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

@inproceedings{heward_supporting_2022,\n\ttitle = {Supporting {Open} {Science} with the {Europlanet} {Research} {Infrastructure}},\n\turl = {https://www.europlanet-society.org/wp-content/uploads/2024/02/232-1.pdf},\n\tlanguage = {en},\n\turldate = {2022-11-30},\n\tpublisher = {Copernicus Meetings},\n\tauthor = {Heward, Anita and DeWitt, Jen},\n\tmonth = jul,\n\tyear = {2022},\n\tdoi = {10.5194/epsc2022-614},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Exoplanet observations: amateur experience from the Europlanet Telescope network.\n \n \n \n \n\n\n \n Libotte, F.; and Correa, M.\n\n\n \n\n\n\n Technical Report EPSC2022-945, Copernicus Meetings, July 2022.\n \n\n\n\n
\n\n\n\n \n \n $\"Exoplanet$ 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

@techreport{libotte_exoplanet_2022,\n\ttitle = {Exoplanet observations: amateur experience from the {Europlanet} {Telescope} network},\n\tshorttitle = {Exoplanet observations},\n\turl = {https://www.europlanet-society.org/wp-content/uploads/2024/02/236-1.pdf},\n\tlanguage = {en},\n\tnumber = {EPSC2022-945},\n\turldate = {2022-11-30},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Libotte, Florence and Correa, Mercè},\n\tmonth = jul,\n\tyear = {2022},\n\tdoi = {10.5194/epsc2022-945},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n High-Altitude Andean Lakes as Natural Laboratories for Planetary Geology and Astrobiology Research: The Laguna Negra case (Argentina).\n \n \n \n \n\n\n \n Gomez, F.; Matic, M.; Perez Valdenegro, P.; Boidi, F.; and Mlewski, C.\n\n\n \n\n\n\n Technical Report display, September 2022.\n \n\n\n\n
\n\n\n\n \n \n $\"High-Altitude$ 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

@techreport{gomez_high-altitude_2022,\n\ttype = {other},\n\ttitle = {High-{Altitude} {Andean} {Lakes} as {Natural} {Laboratories} for {Planetary} {Geology} and {Astrobiology} {Research}: {The} {Laguna} {Negra} case ({Argentina})},\n\tshorttitle = {High-{Altitude} {Andean} {Lakes} as {Natural} {Laboratories} for {Planetary} {Geology} and {Astrobiology} {Research}},\n\turl = {https://www.europlanet-society.org/wp-content/uploads/2024/02/241-1.pdf},\n\tabstract = {\\&lt;p align=\\&quot;justify\\&quot;\\&gt;\\&lt;strong\\&gt;Introduction\\&lt;/strong\\&gt;\\&lt;/p\\&gt;\n\\&lt;p align=\\&quot;justify\\&quot;\\&gt;Sedimentary deposits developed in High-Altitude Andean Lakes (HAAL) share some extreme and environmental characteristics that made them excellent analogues for planetary geology and astrobiology research. These conditions favor the development of a diverse and abundant microbial biota that influence mineral precipitation (e.g. carbonates) and the develpoment of microbially influenced sedimentary deposits typically know as stromatolites. To recognize and differentiate stromatolites from similar laminated deposits purelly formed by chemical processes is not straightforward, and Archean stromatolites are a good example. This makes HAAL good environmental analogues to study microbe-mineral proceeses, and the associated biosignatures. The recent findings of putative marginal lacustrine and delta deposits in the Jezero crater on Mars surface highlight the potential of these systems from and astrobiology perspective. The origin and characteristics of these martian carbonates is still unknown so the evaluation potential scenarios in comparable environmental conditions may shed some light into this uncertainties.\\&lt;/p\\&gt;\n\\&lt;p align=\\&quot;justify\\&quot;\\&gt;The Laguna Negra (a high altitude lake in Catamarca Province, Argentina) is an outstaning example of HAAL where an active microbial mat system and associated carbonate deposits is well developed. These are located in the mixing zone between groundwater spring-fed pools and the main lacustrine system. The Laguna Negra is a unique natural laboratory that fulfills the environmental criteria suggested for early Earth (Archean) and Mars (Noachian) where spectrum of biotic and abiotic process can be studied improving our ability to interpret the sedimentary record on our planet and beyond.\\&lt;/p\\&gt;\n\\&lt;p align=\\&quot;justify\\&quot;\\&gt;\\&lt;strong\\&gt;Geological setting\\&lt;/strong\\&gt;\\&lt;/p\\&gt;\n\\&lt;p align=\\&quot;justify\\&quot;\\&gt;The Laguna Negra is a shallow hypersaline lake where the pH of the main lake and the groundwater springs feeding the lake fluctuates between {\\textasciitilde}6 and {\\textasciitilde}8 and salinity between {\\textasciitilde}320 and {\\textasciitilde}9 ppt respectively. The mixing zone between the main lake and groundwater is oversaturated with respect to calcite and aragonite. The carbonate belt consists of \\&lt;strong\\&gt;oncoids\\&lt;/strong\\&gt;, \\&lt;strong\\&gt;stromatolites\\&lt;/strong\\&gt;, and \\&lt;strong\\&gt;laminar crusts\\&lt;/strong\\&gt; that are spatially localized in different zones and associated to different microbial mats systems and chemical conditions. Particularly interesting are the laminar crusts, developed in a zone where no significant microbial mats has been observed, but where a diversity of morphologies and microtextures has been recorded. Although interpreted as purelly chemically precipitated, unravelling the different processes that controls this morphological varibality is still challenging.\\&lt;/p\\&gt;\n\\&lt;p align=\\&quot;justify\\&quot;\\&gt;\\&lt;strong\\&gt;Oncoids, Stromatolites and Laminar crusts\\&lt;/strong\\&gt;\\&lt;/p\\&gt;\n\\&lt;p align=\\&quot;justify\\&quot;\\&gt;\\&lt;strong\\&gt;Oncoids\\&lt;/strong\\&gt; represented by concentrically laminated discs, spheres, and flattened domes (cm to dm in diameter) that can coalesce to form more complex structures and are typically associated with well-stratified diatom-rich microbial mats. The external surface surface can be smooth or can show pillar-like to shrub-shaped millimeter scale protrusions and ornamentations, particularly on the side affected by wind and currents. Oncoids are partially buried and can show lateral protrusions at the sediment\\&amp;\\#8211;water and the air\\&amp;\\#8211;water interface. Although oncoids are sub-spherical in shape, they can show asymmetric growth (bigger below the sediment\\&amp;\\#8211;water interface). Complex lamination is also a result of oncoid rotation, particularly by cryoturbation and bioturbation.\\&lt;/p\\&gt;\n\\&lt;p align=\\&quot;justify\\&quot;\\&gt;Although water mixing, CO\\&lt;sub\\&gt;2\\&lt;/sub\\&gt; degassing, and evaporation are particularly important to trigger carbonate precipitation the influence of microbial mats is visible in the macromorphologies (differential growth within the anoxic zone related to metabolisms that increase alkalinity) and a diverse set of microtextures some of which are interpreted as microbially influenced.\\&lt;/p\\&gt;\n\\&lt;p align=\\&quot;justify\\&quot;\\&gt;\\&lt;strong\\&gt;Stromatolites\\&lt;/strong\\&gt; more localized and represented by centimeter to decimeter-scale laminated structures (up to 25 cm) that typically have a planar or laminar to columnar shape. They are observed associated with dark colored microbial mats and usually are encrusting the upper surface of oncoids. The columnar structures are usually centimeter-sized. Internal lamination is irregular, overlapping, crenulated-micritic to micro-peloidal laminae that preserve abundant organic remains. These features are suggestive of microbially influenced texture.\\&lt;/p\\&gt;\n\\&lt;p align=\\&quot;justify\\&quot;\\&gt;\\&lt;strong\\&gt;Laminar crusts \\&lt;/strong\\&gt;show a patchy distribution and represented by millimeter to decimeter carbonate crusts encrusting volcanic rocks, peloidal sediments as well as organic remains. Can also develop dome-shaped morphologies showing concentric growth patterns. These concentric structures can be slightly assymetrical, showing preferential growth towards the upper half (as opposed to oncoids). Oriented and elongated structures are common (by wind-driven currents in the lake). Plates and domes can be rotated and/or coalesce to form more complex structures or more extensive platforms along the lakeshore. The surface can be smooth or show dendritic to pustular patterns or protusions as well as travertine-like microterracetes.\\&lt;/p\\&gt;\n\\&lt;p align=\\&quot;justify\\&quot;\\&gt;Isopachous regular laminane is the most common building block, as stated showing a concentric pattern but it is worth mentioning that the wind-oriented structures, in cross-section, develop more complex micro-textures (shrub-like to dendritic/micro-stromatolite microfabrics) that resemble microbially influenced structures.\\&lt;/p\\&gt;\n\\&lt;p align=\\&quot;justify\\&quot;\\&gt;Given the absence of microbial mats, and the macro-morphologies and micro-textures described (e.g., lamina regularity and degree of inheritance, lack of organic remains within the lamina), these structures have been interpreted as predominantly chemically precipitated carbonates, triggered by oversaturation related to water mixing, strong CO2 degassing, and evaporation.\\&lt;/p\\&gt;\n\\&lt;p align=\\&quot;justify\\&quot;\\&gt;\\&lt;strong\\&gt;Final considerations\\&lt;/strong\\&gt;\\&lt;/p\\&gt;\n\\&lt;p align=\\&quot;justify\\&quot;\\&gt;Both, physocochemical and microbial processes can contribute to a diverse range of morphologies and carbonate microtextures and it is not easy to urvanel their relative contributions. Oncoids, stromatolites and laminar crusts show some distinctive features that suggest some of the driving controls, but also some overlapping characteristics that may be difficult to discriminate. As an example, although laminar crusts generally show (in cross section) a strong lamina regularity, a more diverse set of microtextures can be produced by the influence of advective-diffusive processes, localized scarbonate precipitation, rotation due waves, and cryo-bioturbation, thus increasing lamina complexity that can be confused with microbially influenced textures. Possible origins of the carbonates recorded at Jezero crater, for example including carbonate crusts developed over the basaltic substrate, pore-vein-filling carbonate cements, reworked carbonate material, or even stromatolite-like structures. Although chemical biosignatures (trace element distribution and isotope fractionation) are central in the tool box of astrobiologists, to recognize the putative biogenicity of these carbonates it is necessary to combine chemical analysis with the information provided by the external macro-micro morphology and the internal macro and micro microfabric, something that may not be possible when dealing with rover or image based analysis on outcrops or with sample returned to Earth, where part of the context may be lost.\\&lt;/p\\&gt;\n\\&lt;p align=\\&quot;justify\\&quot;\\&gt;\\&amp;\\#160;\\&lt;/p\\&gt;\n\\&lt;p align=\\&quot;justify\\&quot;\\&gt;\\&amp;\\#160;\\&lt;/p\\&gt;},\n\turldate = {2022-11-30},\n\tinstitution = {display},\n\tauthor = {Gomez, Fernando and Matic, Mara and Perez Valdenegro, Paloma and Boidi, Flavia and Mlewski, Cecilia},\n\tmonth = sep,\n\tyear = {2022},\n\tdoi = {10.5194/epsc2022-822},\n}\n\n

\n\n\n

\n Introduction Sedimentary deposits developed in High-Altitude Andean Lakes (HAAL) share some extreme and environmental characteristics that made them excellent analogues for planetary geology and astrobiology research. These conditions favor the development of a diverse and abundant microbial biota that influence mineral precipitation (e.g. carbonates) and the develpoment of microbially influenced sedimentary deposits typically know as stromatolites. To recognize and differentiate stromatolites from similar laminated deposits purelly formed by chemical processes is not straightforward, and Archean stromatolites are a good example. This makes HAAL good environmental analogues to study microbe-mineral proceeses, and the associated biosignatures. The recent findings of putative marginal lacustrine and delta deposits in the Jezero crater on Mars surface highlight the potential of these systems from and astrobiology perspective. The origin and characteristics of these martian carbonates is still unknown so the evaluation potential scenarios in comparable environmental conditions may shed some light into this uncertainties. The Laguna Negra (a high altitude lake in Catamarca Province, Argentina) is an outstaning example of HAAL where an active microbial mat system and associated carbonate deposits is well developed. These are located in the mixing zone between groundwater spring-fed pools and the main lacustrine system. The Laguna Negra is a unique natural laboratory that fulfills the environmental criteria suggested for early Earth (Archean) and Mars (Noachian) where spectrum of biotic and abiotic process can be studied improving our ability to interpret the sedimentary record on our planet and beyond. Geological setting The Laguna Negra is a shallow hypersaline lake where the pH of the main lake and the groundwater springs feeding the lake fluctuates between ~6 and ~8 and salinity between ~320 and ~9 ppt respectively. The mixing zone between the main lake and groundwater is oversaturated with respect to calcite and aragonite. The carbonate belt consists of oncoids, stromatolites, and laminar crusts that are spatially localized in different zones and associated to different microbial mats systems and chemical conditions. Particularly interesting are the laminar crusts, developed in a zone where no significant microbial mats has been observed, but where a diversity of morphologies and microtextures has been recorded. Although interpreted as purelly chemically precipitated, unravelling the different processes that controls this morphological varibality is still challenging. Oncoids, Stromatolites and Laminar crusts Oncoids represented by concentrically laminated discs, spheres, and flattened domes (cm to dm in diameter) that can coalesce to form more complex structures and are typically associated with well-stratified diatom-rich microbial mats. The external surface surface can be smooth or can show pillar-like to shrub-shaped millimeter scale protrusions and ornamentations, particularly on the side affected by wind and currents. Oncoids are partially buried and can show lateral protrusions at the sediment–water and the air–water interface. Although oncoids are sub-spherical in shape, they can show asymmetric growth (bigger below the sediment–water interface). Complex lamination is also a result of oncoid rotation, particularly by cryoturbation and bioturbation. Although water mixing, CO2 degassing, and evaporation are particularly important to trigger carbonate precipitation the influence of microbial mats is visible in the macromorphologies (differential growth within the anoxic zone related to metabolisms that increase alkalinity) and a diverse set of microtextures some of which are interpreted as microbially influenced. Stromatolites more localized and represented by centimeter to decimeter-scale laminated structures (up to 25 cm) that typically have a planar or laminar to columnar shape. They are observed associated with dark colored microbial mats and usually are encrusting the upper surface of oncoids. The columnar structures are usually centimeter-sized. Internal lamination is irregular, overlapping, crenulated-micritic to micro-peloidal laminae that preserve abundant organic remains. These features are suggestive of microbially influenced texture. Laminar crusts show a patchy distribution and represented by millimeter to decimeter carbonate crusts encrusting volcanic rocks, peloidal sediments as well as organic remains. Can also develop dome-shaped morphologies showing concentric growth patterns. These concentric structures can be slightly assymetrical, showing preferential growth towards the upper half (as opposed to oncoids). Oriented and elongated structures are common (by wind-driven currents in the lake). Plates and domes can be rotated and/or coalesce to form more complex structures or more extensive platforms along the lakeshore. The surface can be smooth or show dendritic to pustular patterns or protusions as well as travertine-like microterracetes. Isopachous regular laminane is the most common building block, as stated showing a concentric pattern but it is worth mentioning that the wind-oriented structures, in cross-section, develop more complex micro-textures (shrub-like to dendritic/micro-stromatolite microfabrics) that resemble microbially influenced structures. Given the absence of microbial mats, and the macro-morphologies and micro-textures described (e.g., lamina regularity and degree of inheritance, lack of organic remains within the lamina), these structures have been interpreted as predominantly chemically precipitated carbonates, triggered by oversaturation related to water mixing, strong CO2 degassing, and evaporation. Final considerations Both, physocochemical and microbial processes can contribute to a diverse range of morphologies and carbonate microtextures and it is not easy to urvanel their relative contributions. Oncoids, stromatolites and laminar crusts show some distinctive features that suggest some of the driving controls, but also some overlapping characteristics that may be difficult to discriminate. As an example, although laminar crusts generally show (in cross section) a strong lamina regularity, a more diverse set of microtextures can be produced by the influence of advective-diffusive processes, localized scarbonate precipitation, rotation due waves, and cryo-bioturbation, thus increasing lamina complexity that can be confused with microbially influenced textures. Possible origins of the carbonates recorded at Jezero crater, for example including carbonate crusts developed over the basaltic substrate, pore-vein-filling carbonate cements, reworked carbonate material, or even stromatolite-like structures. Although chemical biosignatures (trace element distribution and isotope fractionation) are central in the tool box of astrobiologists, to recognize the putative biogenicity of these carbonates it is necessary to combine chemical analysis with the information provided by the external macro-micro morphology and the internal macro and micro microfabric, something that may not be possible when dealing with rover or image based analysis on outcrops or with sample returned to Earth, where part of the context may be lost.    \n

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\n \n\n \n \n \n \n \n \n Automatic Detection and Classification of Boundary Crossings in Spacecraft in situ Data.\n \n \n \n \n\n\n \n Rüdisser, H. T.; Windisch, A.; Amerstorfer, U. V.; Píša, D.; and Soucek, J.\n\n\n \n\n\n\n Technical Report EPSC2022-47, Copernicus Meetings, July 2022.\n \n\n\n\n
\n\n\n\n \n \n $\"Automatic$ 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

@techreport{rudisser_automatic_2022,\n\ttitle = {Automatic {Detection} and {Classification} of {Boundary} {Crossings} in {Spacecraft} in situ {Data}},\n\turl = {Automatic Detection and Classification of Boundary Crossings in Spacecraft in situ Data},\n\tlanguage = {en},\n\tnumber = {EPSC2022-47},\n\turldate = {2023-06-28},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Rüdisser, Hannah Theresa and Windisch, Andreas and Amerstorfer, Ute V. and Píša, David and Soucek, Jan},\n\tmonth = jul,\n\tyear = {2022},\n\tdoi = {10.5194/epsc2022-47},\n}\n\n

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\n \n\n \n \n \n \n \n \n EPN-TAP: Publishing Solar System Data to the Virtual Observatory Version 2.0.\n \n \n \n \n\n\n \n Erard, S.; Cecconi, B.; Le Sidaner, P.; Demleitner, M.; and Taylor, M.\n\n\n \n\n\n\n IVOA Recommendation 22 August 2022,822. August 2022.\n ADS Bibcode: 2022ivoa.spec.0822E\n\n\n\n
\n\n\n\n \n \n $\"EPN-TAP:$ 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{erard_epn-tap_2022,\n\ttitle = {{EPN}-{TAP}: {Publishing} {Solar} {System} {Data} to the {Virtual} {Observatory} {Version} 2.0},\n\tshorttitle = {{EPN}-{TAP}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2022ivoa.spec.0822E},\n\tabstract = {This document defines the EPN-TAP framework, which is using TAP with the EPNCore metadata dictionary. The EPNCore metadata dictionary defines the core components that are necessary to perform data discovery in the Solar System related science fields. It includes parameters to describe data products coverage (temporal, spectral, spatial, photometric), origin (instrument, facility), content (target, physical parameters), access, references, etc. Its implementation with TAP (Table Access Protocol) is presented, including service registration guidelines. Topical extension metadata dictionaries are also presented.},\n\turldate = {2023-09-22},\n\tjournal = {IVOA Recommendation 22 August 2022},\n\tauthor = {Erard, Stéphane and Cecconi, Baptiste and Le Sidaner, Pierre and Demleitner, Markus and Taylor, Mark},\n\tmonth = aug,\n\tyear = {2022},\n\tnote = {ADS Bibcode: 2022ivoa.spec.0822E},\n\tpages = {822},\n}\n\n

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\n \n\n \n \n \n \n \n \n Automated surface mapping via unsupervised learning and classification of Mercury Visible–Near-Infrared reflectance spectra.\n \n \n \n \n\n\n \n D'Amore, M.; and Padovan, S.\n\n\n \n\n\n\n In Machine Learning for Planetary Science, pages 131–149. Elsevier, January 2022.\n \n\n\n\n
\n\n\n\n \n \n $\"Automated$ 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

@incollection{damore_automated_2022,\n\ttitle = {Automated surface mapping via unsupervised learning and classification of {Mercury} {Visible}–{Near}-{Infrared} reflectance spectra},\n\turl = {http://www.sciencedirect.com/science/article/abs/pii/B9780128187210000161},\n\tabstract = {In this work we apply unsupervised learning techniques for dimensionality reduction and clustering to remote sensing hyperspectral Visible-Near Infrar…},\n\tlanguage = {en-US},\n\turldate = {2023-08-08},\n\tbooktitle = {Machine {Learning} for {Planetary} {Science}},\n\tpublisher = {Elsevier},\n\tauthor = {D'Amore, M. and Padovan, S.},\n\tmonth = jan,\n\tyear = {2022},\n\tdoi = {10.1016/B978-0-12-818721-0.00016-1},\n\tpages = {131--149},\n}\n\n

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\n \n\n \n \n \n \n \n \n A search for transit timing variations in the HATS-18 planetary system.\n \n \n \n \n\n\n \n Southworth, J.; Barker, A J; Hinse, T C; Jongen, Y; Dominik, M; Jørgensen, U G; Longa-Peña, P; Sajadian, S; Snodgrass, C; Tregloan-Reed, J; Bach-Møller, N; Bonavita, M; Bozza, V; Burgdorf, M J; Figuera Jaimes, R; Helling, C.; Hitchcock, J A; Hundertmark, M; Khalouei, E; Korhonen, H; Mancini, L; Peixinho, N; Rahvar, S; Rabus, M; Skottfelt, J; and Spyratos, P\n\n\n \n\n\n\n Monthly Notices of the Royal Astronomical Society, 515(3): 3212–3223. August 2022.\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{southworth_search_2022,\n\ttitle = {A search for transit timing variations in the {HATS}-18 planetary system},\n\tvolume = {515},\n\tissn = {0035-8711, 1365-2966},\n\turl = {https://academic.oup.com/mnras/article/515/3/3212/6640422},\n\tdoi = {10.1093/mnras/stac1931},\n\tabstract = {ABSTRACT \n            HATS-18 b is a transiting planet with a large mass and a short orbital period, and is one of the best candidates for the detection of orbital decay induced by tidal effects. We present extensive photometry of HATS-18 from which we measure 27 times of mid-transit. Two further transit times were measured from data from the Transiting Exoplanet Survey Satellite (TESS) and three more taken from the literature. The transit timings were fitted with linear and quadratic ephemerides and an upper limit on orbital decay was determined. This corresponds to a lower limit on the modified stellar tidal quality factor of \\$Q\\_{\\textbackslash}star {\\textasciicircum}\\{{\\textbackslash}, {\\textbackslash}prime \\} {\\textbackslash}gt 10{\\textasciicircum}\\{5.11 {\\textbackslash}pm 0.04\\}\\$. This is at the cusp of constraining the presence of enhanced tidal dissipation due to internal gravity waves. We also refine the measured physical properties of the HATS-18 system, place upper limits on the masses of third bodies, and compare the relative performance of TESS and the 1.54 m Danish Telescope in measuring transit times for this system.},\n\tlanguage = {en},\n\tnumber = {3},\n\turldate = {2023-06-26},\n\tjournal = {Monthly Notices of the Royal Astronomical Society},\n\tauthor = {Southworth, John and Barker, A J and Hinse, T C and Jongen, Y and Dominik, M and Jørgensen, U G and Longa-Peña, P and Sajadian, S and Snodgrass, C and Tregloan-Reed, J and Bach-Møller, N and Bonavita, M and Bozza, V and Burgdorf, M J and Figuera Jaimes, R and Helling, Ch and Hitchcock, J A and Hundertmark, M and Khalouei, E and Korhonen, H and Mancini, L and Peixinho, N and Rahvar, S and Rabus, M and Skottfelt, J and Spyratos, P},\n\tmonth = aug,\n\tyear = {2022},\n\tpages = {3212--3223},\n}\n\n

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\n \n\n \n \n \n \n \n \n Amateur Observers Witness the Return of Venus’ Cloud Discontinuity.\n \n \n \n \n\n\n \n Kardasis, E. (.; Peralta, J.; Maravelias, G.; Imai, M.; Wesley, A.; Olivetti, T.; Naryzhniy, Y.; Morrone, L.; Gallardo, A.; Calapai, G.; Camarena, J.; Casquinha, P.; Kananovich, D.; MacNeill, N.; Viladrich, C.; and Takoudi, A.\n\n\n \n\n\n\n Atmosphere, 13(2): 348. February 2022.\n \n\n\n\n
\n\n\n\n \n \n $\"Amateur$ 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{kardasis_amateur_2022,\n\ttitle = {Amateur {Observers} {Witness} the {Return} of {Venus}’ {Cloud} {Discontinuity}},\n\tvolume = {13},\n\tcopyright = {http://creativecommons.org/licenses/by/3.0/},\n\tissn = {2073-4433},\n\turl = {https://www.mdpi.com/2073-4433/13/2/348},\n\tdoi = {10.3390/atmos13020348},\n\tabstract = {Firstly identified in images from JAXA’s orbiter Akatsuki, the cloud discontinuity of Venus is a planetary-scale phenomenon known to be recurrent since, at least, the 1980s. Interpreted as a new type of Kelvin wave, this disruption is associated to dramatic changes in the clouds’ opacity and distribution of aerosols, and it may constitute a critical piece for our understanding of the thermal balance and atmospheric circulation of Venus. Here, we report its reappearance on the dayside middle clouds four years after its last detection with Akatsuki/IR1, and for the first time, we characterize its main properties using exclusively near-infrared images from amateur observations. In agreement with previous reports, the discontinuity exhibited temporal variations in its zonal speed, orientation, length, and its effect over the clouds’ albedo during the 2019/2020 eastern elongation. Finally, a comparison with simultaneous observations by Akatsuki UVI and LIR confirmed that the discontinuity is not visible on the upper clouds’ albedo or thermal emission, while zonal speeds are slower than winds at the clouds’ top and faster than at the middle clouds, evidencing that this Kelvin wave might be transporting momentum up to upper clouds.},\n\tlanguage = {en},\n\tnumber = {2},\n\turldate = {2023-06-26},\n\tjournal = {Atmosphere},\n\tauthor = {Kardasis, Emmanuel (Manos) and Peralta, Javier and Maravelias, Grigoris and Imai, Masataka and Wesley, Anthony and Olivetti, Tiziano and Naryzhniy, Yaroslav and Morrone, Luigi and Gallardo, Antonio and Calapai, Giovanni and Camarena, Joaquin and Casquinha, Paulo and Kananovich, Dzmitry and MacNeill, Niall and Viladrich, Christian and Takoudi, Alexia},\n\tmonth = feb,\n\tyear = {2022},\n\tkeywords = {Venus, atmosphere, atmospheric dynamics, atmospheric waves, terrestrial planets},\n\tpages = {348},\n}\n\n

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

\n\n\n

\n \n\n \n \n \n \n \n \n Mid-IR and VUV spectroscopic characterisation of thermally processed and electron irradiated CO2 astrophysical ice analogues.\n \n \n \n \n\n\n \n Mifsud, D.; Kaňuchová, Z.; Ioppolo, S.; Herczku, P.; Traspas Muiña, A.; Field, T.; Hailey, P.; Juhász, Z.; Kovács, S.; Mason, N.; McCullough, R.; Pavithraa, S.; Rahul, K.; Paripás, B.; Sulik, B.; Chou, S.; Lo, J.; Das, A.; Cheng, B.; Rajasekhar, B.; Bhardwaj, A.; and Sivaraman, B.\n\n\n \n\n\n\n Journal of Molecular Spectroscopy, 385: 111599. March 2022.\n \n\n\n\n
\n\n\n\n \n \n $\"Mid-IR$ 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\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{mifsud_mid-ir_2022,\n\ttitle = {Mid-{IR} and {VUV} spectroscopic characterisation of thermally processed and electron irradiated {CO2} astrophysical ice analogues},\n\tvolume = {385},\n\tissn = {00222852},\n\turl = {https://linkinghub.elsevier.com/retrieve/pii/S002228522200025X},\n\tdoi = {10.1016/j.jms.2022.111599},\n\tlanguage = {en},\n\turldate = {2023-06-26},\n\tjournal = {Journal of Molecular Spectroscopy},\n\tauthor = {Mifsud, D.V. and Kaňuchová, Z. and Ioppolo, S. and Herczku, P. and Traspas Muiña, A. and Field, T.A. and Hailey, P.A. and Juhász, Z. and Kovács, S.T.S. and Mason, N.J. and McCullough, R.W. and Pavithraa, S. and Rahul, K.K. and Paripás, B. and Sulik, B. and Chou, S.-L. and Lo, J.-I. and Das, A. and Cheng, B.-M. and Rajasekhar, B.N. and Bhardwaj, A. and Sivaraman, B.},\n\tmonth = mar,\n\tyear = {2022},\n\tpages = {111599},\n}\n\n

\n\n\n\n

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\n \n\n \n \n \n \n \n \n Ozone production in electron irradiated CO2:O2 ices.\n \n \n \n \n\n\n \n Mifsud, D. V.; Kaňuchová, Z.; Ioppolo, S.; Herczku, P.; Muiña, A. T.; Sulik, B.; Rahul, K. K.; Kovács, S. T. S.; Hailey, P. A.; McCullough, R. W.; Mason, N. J.; and Juhász, Z.\n\n\n \n\n\n\n Physical Chemistry Chemical Physics, 24(30): 18169–18178. August 2022.\n \n\n\n\n
\n\n\n\n \n \n $\"Ozone$ 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{mifsud_ozone_2022,\n\ttitle = {Ozone production in electron irradiated {CO2}:{O2} ices},\n\tvolume = {24},\n\tissn = {1463-9084},\n\tshorttitle = {Ozone production in electron irradiated {CO2}},\n\turl = {https://pubs.rsc.org/en/content/articlelanding/2022/cp/d2cp01535h},\n\tdoi = {10.1039/D2CP01535H},\n\tabstract = {The detection of ozone (O3) in the surface ices of Ganymede, Jupiter's largest moon, and of the Saturnian moons Rhea and Dione, has motivated several studies on the route of formation of this species. Previous studies have successfully quantified trends in the production of O3 as a result of the irradiation of pure molecular ices using ultraviolet photons and charged particles (i.e., ions and electrons), such as the abundances of O3 formed after irradiation at different temperatures or using different charged particles. In this study, we extend such results by quantifying the abundance of O3 as a result of the 1 keV electron irradiation of a series of 14 stoichiometrically distinct CO2:O2 astrophysical ice analogues at 20 K. By using mid-infrared spectroscopy as our primary analytical tool, we have also been able to perform a spectral analysis of the asymmetric stretching mode of solid O3 and the variation in its observed shape and profile among the investigated ice mixtures. Our results are important in the context of better understanding the surface composition and chemistry of icy outer Solar System objects, and may thus be of use to future interplanetary space missions such as the ESA Jupiter Icy Moons Explorer and the NASA Europa Clipper missions, as well as the recently launched NASA James Webb Space Telescope.},\n\tlanguage = {en},\n\tnumber = {30},\n\turldate = {2023-06-26},\n\tjournal = {Physical Chemistry Chemical Physics},\n\tauthor = {Mifsud, Duncan V. and Kaňuchová, Zuzana and Ioppolo, Sergio and Herczku, Péter and Muiña, Alejandra Traspas and Sulik, Béla and Rahul, K. K. and Kovács, Sándor T. S. and Hailey, Perry A. and McCullough, Robert W. and Mason, Nigel J. and Juhász, Zoltán},\n\tmonth = aug,\n\tyear = {2022},\n\tpages = {18169--18178},\n}\n\n

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\n \n\n \n \n \n \n \n \n Comparative electron irradiations of amorphous and crystalline astrophysical ice analogues.\n \n \n \n \n\n\n \n Mifsud, D. V.; Hailey, P. A.; Herczku, P.; Sulik, B.; Juhász, Z.; Kovács, S. T. S.; Kaňuchová, Z.; Ioppolo, S.; McCullough, R. W.; Paripás, B.; and Mason, N. J.\n\n\n \n\n\n\n Physical Chemistry Chemical Physics, 24(18): 10974–10984. May 2022.\n \n\n\n\n
\n\n\n\n \n \n $\"Comparative$ 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{mifsud_comparative_2022,\n\ttitle = {Comparative electron irradiations of amorphous and crystalline astrophysical ice analogues},\n\tvolume = {24},\n\tissn = {1463-9084},\n\turl = {https://pubs.rsc.org/en/content/articlelanding/2022/cp/d2cp00886f},\n\tdoi = {10.1039/D2CP00886F},\n\tabstract = {Laboratory studies of the radiation chemistry occurring in astrophysical ices have demonstrated the dependence of this chemistry on a number of experimental parameters. One experimental parameter which has received significantly less attention is that of the phase of the solid ice under investigation. In this present study, we have performed systematic 2 keV electron irradiations of the amorphous and crystalline phases of pure CH3OH and N2O astrophysical ice analogues. Radiation-induced decay of these ices and the concomitant formation of products were monitored in situ using FT-IR spectroscopy. A direct comparison between the irradiated amorphous and crystalline CH3OH ices revealed a more rapid decay of the former compared to the latter. Interestingly, a significantly lesser difference was observed when comparing the decay rates of the amorphous and crystalline N2O ices. These observations have been rationalised in terms of the strength and extent of the intermolecular forces present in each ice. The strong and extensive hydrogen-bonding network that exists in crystalline CH3OH (but not in the amorphous phase) is suggested to significantly stabilise this phase against radiation-induced decay. Conversely, although alignment of the dipole moment of N2O is anticipated to be more extensive in the crystalline structure, its weak attractive potential does not significantly stabilise the crystalline phase against radiation-induced decay, hence explaining the smaller difference in decay rates between the amorphous and crystalline phases of N2O compared to those of CH3OH. Our results are relevant to the astrochemistry of interstellar ices and icy Solar System objects, which may experience phase changes due to thermally-induced crystallisation or space radiation-induced amorphisation.},\n\tlanguage = {en},\n\tnumber = {18},\n\turldate = {2023-06-26},\n\tjournal = {Physical Chemistry Chemical Physics},\n\tauthor = {Mifsud, Duncan V. and Hailey, Perry A. and Herczku, Péter and Sulik, Béla and Juhász, Zoltán and Kovács, Sándor T. S. and Kaňuchová, Zuzana and Ioppolo, Sergio and McCullough, Robert W. and Paripás, Béla and Mason, Nigel J.},\n\tmonth = may,\n\tyear = {2022},\n\tpages = {10974--10984},\n}\n\n

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\n \n\n \n \n \n \n \n \n Laboratory experiments on the radiation astrochemistry of water ice phases.\n \n \n \n \n\n\n \n Mifsud, D. V.; Hailey, P. A.; Herczku, P.; Juhász, Z.; Kovács, S. T. S.; Sulik, B.; Ioppolo, S.; Kaňuchová, Z.; McCullough, R. W.; Paripás, B.; and Mason, N. J.\n\n\n \n\n\n\n The European Physical Journal D, 76(5): 87. May 2022.\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{mifsud_laboratory_2022,\n\ttitle = {Laboratory experiments on the radiation astrochemistry of water ice phases},\n\tvolume = {76},\n\tissn = {1434-6079},\n\turl = {https://doi.org/10.1140/epjd/s10053-022-00416-4},\n\tdoi = {10.1140/epjd/s10053-022-00416-4},\n\tabstract = {Water (H2O) ice is a ubiquitous component of the universe, having been detected in a variety of interstellar and Solar System environments where radiation plays an important role in its physico-chemical transformations. Although the radiation chemistry of H2O astrophysical ice analogues has been well studied, direct and systematic comparisons of different solid phases are scarce and are typically limited to just two phases. In this article, we describe the results of an in-depth study of the 2 keV electron irradiation of amorphous solid water (ASW), restrained amorphous ice (RAI) and the cubic (Ic) and hexagonal (Ih) crystalline phases at 20 K so as to further uncover any potential dependence of the radiation physics and chemistry on the solid phase of the ice. Mid-infrared spectroscopic analysis of the four investigated H2O ice phases revealed that electron irradiation of the RAI, Ic, and Ih phases resulted in their amorphization (with the latter undergoing the process more slowly) while ASW underwent compaction. The abundance of hydrogen peroxide (H2O2) produced as a result of the irradiation was also found to vary between phases, with yields being highest in irradiated ASW. This observation is the cumulative result of several factors including the increased porosity and quantity of lattice defects in ASW, as well as its less extensive hydrogen-bonding network. Our results have astrophysical implications, particularly with regards to H2O-rich icy interstellar and Solar System bodies exposed to both radiation fields and temperature gradients.},\n\tlanguage = {en},\n\tnumber = {5},\n\turldate = {2023-06-26},\n\tjournal = {The European Physical Journal D},\n\tauthor = {Mifsud, Duncan V. and Hailey, Perry A. and Herczku, Péter and Juhász, Zoltán and Kovács, Sándor T. S. and Sulik, Béla and Ioppolo, Sergio and Kaňuchová, Zuzana and McCullough, Robert W. and Paripás, Béla and Mason, Nigel J.},\n\tmonth = may,\n\tyear = {2022},\n\tpages = {87},\n}\n\n

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\n \n\n \n \n \n \n \n \n Meteoroids as a Source for Mercury's exosphere.\n \n \n \n \n\n\n \n Moroni, M.; Milillo, A.; Mura, A.; Andre, N.; Mangano, V.; Plainaki, C.; Alberti, T.; Orsini, S.; Massetti, S.; Aronica, A.; De Angelis, E.; Rispoli, R.; Sordini, R.; and Kazakov, A.\n\n\n \n\n\n\n July 2022.\n ADS Bibcode: 2022cosp...44..476M\n\n\n\n
\n\n\n\n \n \n $\"Meteoroids$ 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

@misc{moroni_meteoroids_2022,\n\ttitle = {Meteoroids as a {Source} for {Mercury}'s exosphere},\n\turl = {https://ui.adsabs.harvard.edu/abs/2022cosp...44..476M},\n\tabstract = {The study of the meteoroid environment for particles with masses in the 1 μg - 10 g range is relevant to planetary science, space weathering of airless bodies and their upper atmospheric chemistry. For the case of airless bodies as Mercury, meteoroids hit their surfaces directly, producing impact debris and contributing to shape their thin exospheres. Mercury is a unique case in the solar system: absence of an atmosphere and the weakness of the intrinsic magnetic field. The Hermean exosphere is continuously eroded and refilled by interactions between plasma and surface, so the environment is considered as a single, unified system surface- exosphere-magnetosphere. The study of the generation mechanisms, the compositions and the configuration of the Hermean exosphere will provide crucial insight in the planet status and evolution. A global description of planet's exosphere is still not available: missions visited Mercury and added a consistent amount of data, but still the actual knowledge about the morphology of this tenuous atmosphere is anyway poor. This work is focused on study and modelling of the Mercury's exosphere formation throught the process of Micro-Meteoroids Impact Vaporization (MMIV) from the planetary surface. We provide a detailed Ca-source extraction model simulating the expected 3-D Calcium density distribution in Mercury's exosphere due to the MIV mechanism. A prototype of the Virtual Activity (VA) SPIDER (Sun-Planet Interactions Digital Environment on Request) services is used as a Monte Carlo three-dimensional model of the Hermean exosphere to simulate the bombardment of Mercury's surface by micrometeorites from different sources, as Jupiter Family Comets (JFCs), Main Belt Asteroids (MBA), Halley Type and Oort Cloud Comets (HTCs and OCCs), and to analyze particles ejected. We study how the impact vapor varies with heliocentric distance and the high impact velocity of these particles makes them critical for the morphology of the Mercury exosphere, demonstrating a persistent enhancement of the dust/meteoroid at dawn, which should be responsible of the dawn-dusk asymmetry in Mercury's Ca exosphere. The assumed physical parameters of these Mercury-impacting grains are examined for consistency with the observations data. Furthermore, considering that Mercury is the target of the ESA BepiColombo mission, that will study Mercury orbiting around the planet from 2025, it is important to have a modelling tool ready for interpreting observational data and the results presented in this paper can be useful in the exosphere observations planning for the mission. The Sun Planet Interactions Digital Environment on Request (SPIDER) Virtual Activity of the Europlanet H2024 Research Infrastucture is funded by the European Union's Horizon 2020 research and innovation programme under grant agreement No 871149},\n\turldate = {2023-02-25},\n\tauthor = {Moroni, Martina and Milillo, Anna and Mura, Alessandro and Andre, Nicolas and Mangano, Valeria and Plainaki, Christina and Alberti, Tommaso and Orsini, Stefano and Massetti, Stefano and Aronica, Alessandro and De Angelis, Elisabetta and Rispoli, Rosanna and Sordini, Roberto and Kazakov, Adrian},\n\tmonth = jul,\n\tyear = {2022},\n\tnote = {ADS Bibcode: 2022cosp...44..476M},\n}\n\n

\n\n\n

\n The study of the meteoroid environment for particles with masses in the 1 μg - 10 g range is relevant to planetary science, space weathering of airless bodies and their upper atmospheric chemistry. For the case of airless bodies as Mercury, meteoroids hit their surfaces directly, producing impact debris and contributing to shape their thin exospheres. Mercury is a unique case in the solar system: absence of an atmosphere and the weakness of the intrinsic magnetic field. The Hermean exosphere is continuously eroded and refilled by interactions between plasma and surface, so the environment is considered as a single, unified system surface- exosphere-magnetosphere. The study of the generation mechanisms, the compositions and the configuration of the Hermean exosphere will provide crucial insight in the planet status and evolution. A global description of planet's exosphere is still not available: missions visited Mercury and added a consistent amount of data, but still the actual knowledge about the morphology of this tenuous atmosphere is anyway poor. This work is focused on study and modelling of the Mercury's exosphere formation throught the process of Micro-Meteoroids Impact Vaporization (MMIV) from the planetary surface. We provide a detailed Ca-source extraction model simulating the expected 3-D Calcium density distribution in Mercury's exosphere due to the MIV mechanism. A prototype of the Virtual Activity (VA) SPIDER (Sun-Planet Interactions Digital Environment on Request) services is used as a Monte Carlo three-dimensional model of the Hermean exosphere to simulate the bombardment of Mercury's surface by micrometeorites from different sources, as Jupiter Family Comets (JFCs), Main Belt Asteroids (MBA), Halley Type and Oort Cloud Comets (HTCs and OCCs), and to analyze particles ejected. We study how the impact vapor varies with heliocentric distance and the high impact velocity of these particles makes them critical for the morphology of the Mercury exosphere, demonstrating a persistent enhancement of the dust/meteoroid at dawn, which should be responsible of the dawn-dusk asymmetry in Mercury's Ca exosphere. The assumed physical parameters of these Mercury-impacting grains are examined for consistency with the observations data. Furthermore, considering that Mercury is the target of the ESA BepiColombo mission, that will study Mercury orbiting around the planet from 2025, it is important to have a modelling tool ready for interpreting observational data and the results presented in this paper can be useful in the exosphere observations planning for the mission. The Sun Planet Interactions Digital Environment on Request (SPIDER) Virtual Activity of the Europlanet H2024 Research Infrastucture is funded by the European Union's Horizon 2020 research and innovation programme under grant agreement No 871149\n

\n\n\n

\n \n\n \n \n \n \n \n Virtual european solar & planetary access (VESPA) 2022: Sustainability.\n \n \n \n\n\n \n Erard, S.\n\n\n \n\n\n\n In European planetary science congress, pages EPSC2022–676, September 2022. \n tex.adsnote: Provided by the SAO/NASA Astrophysics Data System tex.adsurl: https://ui.adsabs.harvard.edu/abs/2022EPSC...16..676E tex.eid: EPSC2022-676\n\n\n\n
\n\n\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

@inproceedings{2022EPSC...16..676E,\n\ttitle = {Virtual european solar \\& planetary access ({VESPA}) 2022: {Sustainability}},\n\tdoi = {10.5194/epsc2022-676},\n\tbooktitle = {European planetary science congress},\n\tauthor = {Erard, Stéphane},\n\tmonth = sep,\n\tyear = {2022},\n\tnote = {tex.adsnote: Provided by the SAO/NASA Astrophysics Data System\ntex.adsurl: https://ui.adsabs.harvard.edu/abs/2022EPSC...16..676E\ntex.eid: EPSC2022-676},\n\tpages = {EPSC2022--676},\n}\n\n

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\n \n\n \n \n \n \n \n Open‐source planetary data processing environments based on JupyterHub and Docker containers.\n \n \n \n\n\n \n Nodjoumi, G.; Brandt, C.; and Rossi, A. P.\n\n\n \n\n\n\n In 2022. Planetary Science Informatics and Data Analytics Conference\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{nodjoumi_opensource_2022,\n\ttitle = {Open‐source planetary data processing environments based on {JupyterHub} and {Docker} containers},\n\tpublisher = {Planetary Science Informatics and Data Analytics Conference},\n\tauthor = {Nodjoumi, Giacomo and Brandt, Carlos and Rossi, Angelo Pio},\n\tyear = {2022},\n}\n\n

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\n \n\n \n \n \n \n \n \n Convective storms in closed cyclones in Jupiter: (II) numerical modeling.\n \n \n \n \n\n\n \n Iñurrigarro, P.; Hueso, R.; Sánchez-Lavega, A.; and Legarreta, J.\n\n\n \n\n\n\n Icarus, 386: 115169. November 2022.\n \n\n\n\n
\n\n\n\n \n \n $\"Convective$ 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{inurrigarro_convective_2022,\n\ttitle = {Convective storms in closed cyclones in {Jupiter}: ({II}) numerical modeling},\n\tvolume = {386},\n\tissn = {00191035},\n\tshorttitle = {Convective storms in closed cyclones in {Jupiter}},\n\turl = {https://linkinghub.elsevier.com/retrieve/pii/S0019103522002718},\n\tdoi = {10.1016/j.icarus.2022.115169},\n\tlanguage = {en},\n\turldate = {2023-02-28},\n\tjournal = {Icarus},\n\tauthor = {Iñurrigarro, Peio and Hueso, Ricardo and Sánchez-Lavega, Agustín and Legarreta, Jon},\n\tmonth = nov,\n\tyear = {2022},\n\tpages = {115169},\n}\n\n

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\n \n\n \n \n \n \n \n \n Micro-meteoroids impact vaporization (MMIV) as source for Ca and CaO exosphere along Mercury's orbit.\n \n \n \n \n\n\n \n Moroni, M.; Milillo, A.; Mura, A.; André, N.; Plainaki, C.; Mangano, V.; Massetti, S.; Orsini, S.; Aronica, A.; De Angelis, E.; Rispoli, R.; Sordini, R.; Kazakov, A.; and Del Moro, D.\n\n\n \n\n\n\n June 2022.\n ADS Bibcode: 2022merc.conf...40M\n\n\n\n
\n\n\n\n \n \n $\"Micro-meteoroids$ 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 \n \n \n \n \n\n\n\n

@book{moroni_micro-meteoroids_2022,\n\ttitle = {Micro-meteoroids impact vaporization ({MMIV}) as source for {Ca} and {CaO} exosphere along {Mercury}'s orbit},\n\turl = {https://ui.adsabs.harvard.edu/abs/2022merc.conf...40M},\n\tabstract = {The study of the micro-meteoroid environment is relevant to planetary science, space weathering of airless bodies, as Mercury, and their upper atmospheric chemistry. In this case, the meteoroids hit directly the surface without any interaction with the atmospheric particles, producing impact debris and contributing to shape its thin exosphere. The study of the generation mechanisms, the compositions and the configuration of the Hermean exosphere will provide crucial insight in the planet status and evolution. This work is focused on study and modelling of the Mercury's exosphere formation through the process of Micro-Meteoroids Impact Vaporization (MMIV) from the planetary surface. The MESSENGER/NASA mission visited Mercury in the period 2008-2015, providing measurements of unprecedented quality of Mercury's exosphere, which permit the study of the seasonal variations of metals like Calcium. The Ca in Mercury's exosphere exhibited very high energies, with a scale height consistent with a temperature {\\textgreater} 20,000 K, seen mainly on the dawnside of the planet. The origin of this high-energy, asymmetric source is unknown. The generating mechanism is believed to be a combination of different processes including the release of atomic and molecular surface particles and the photodissociation of exospheric molecules. In this paper we work on models of Mercury's impactors: we provide a detailed Ca-source extraction model simulating the expected 3-D Ca density distribution in Mercury's exosphere due to the MIV mechanism. A prototype of the Virtual Activity (VA) SPIDER (Sun-Planet Interactions Digital Environment on Request) services is used as a Monte Carlo three-dimensional model of the Hermean exosphere to simulate the bombardment of Mercury's surface by micrometeorites and to analyze particles ejected. We study how the impact vapor varies with heliocentric distance and compare the results to the MESSENGER observations. The morphology of Mercury's Ca and CaO exosphere is in good agreement with the observed Ca along the orbit, excluding specific events like comet stream crossing. The results presented in this work will be useful for the exosphere observations planning and for the data interpretation in the frame of the ESA/JAXA BepiColombo mission, that will study Mercury orbiting around the planet from 2025. More specifically, the resulting molecular distributions will be compared to the measurements of the SERENA-STROFIO mass spectrometer that will be the only instrument able to identify the molecular components. The Sun Planet Interactions Digital Environment on Request (SPIDER) Virtual Activity of the Europlanet H2024 Research Infrastucture is funded by the European Union's Horizon 2020 research and innovation programme under grant agreement No 871149.},\n\turldate = {2023-02-25},\n\tauthor = {Moroni, M. and Milillo, A. and Mura, A. and André, N. and Plainaki, C. and Mangano, V. and Massetti, S. and Orsini, S. and Aronica, A. and De Angelis, E. and Rispoli, R. and Sordini, R. and Kazakov, A. and Del Moro, D.},\n\tmonth = jun,\n\tyear = {2022},\n\tnote = {ADS Bibcode: 2022merc.conf...40M},\n\tkeywords = {Exosphere, Mercury, dynamics, magnetosphere},\n}\n\n

\n\n\n

\n The study of the micro-meteoroid environment is relevant to planetary science, space weathering of airless bodies, as Mercury, and their upper atmospheric chemistry. In this case, the meteoroids hit directly the surface without any interaction with the atmospheric particles, producing impact debris and contributing to shape its thin exosphere. The study of the generation mechanisms, the compositions and the configuration of the Hermean exosphere will provide crucial insight in the planet status and evolution. This work is focused on study and modelling of the Mercury's exosphere formation through the process of Micro-Meteoroids Impact Vaporization (MMIV) from the planetary surface. The MESSENGER/NASA mission visited Mercury in the period 2008-2015, providing measurements of unprecedented quality of Mercury's exosphere, which permit the study of the seasonal variations of metals like Calcium. The Ca in Mercury's exosphere exhibited very high energies, with a scale height consistent with a temperature \\textgreater 20,000 K, seen mainly on the dawnside of the planet. The origin of this high-energy, asymmetric source is unknown. The generating mechanism is believed to be a combination of different processes including the release of atomic and molecular surface particles and the photodissociation of exospheric molecules. In this paper we work on models of Mercury's impactors: we provide a detailed Ca-source extraction model simulating the expected 3-D Ca density distribution in Mercury's exosphere due to the MIV mechanism. A prototype of the Virtual Activity (VA) SPIDER (Sun-Planet Interactions Digital Environment on Request) services is used as a Monte Carlo three-dimensional model of the Hermean exosphere to simulate the bombardment of Mercury's surface by micrometeorites and to analyze particles ejected. We study how the impact vapor varies with heliocentric distance and compare the results to the MESSENGER observations. The morphology of Mercury's Ca and CaO exosphere is in good agreement with the observed Ca along the orbit, excluding specific events like comet stream crossing. The results presented in this work will be useful for the exosphere observations planning and for the data interpretation in the frame of the ESA/JAXA BepiColombo mission, that will study Mercury orbiting around the planet from 2025. More specifically, the resulting molecular distributions will be compared to the measurements of the SERENA-STROFIO mass spectrometer that will be the only instrument able to identify the molecular components. The Sun Planet Interactions Digital Environment on Request (SPIDER) Virtual Activity of the Europlanet H2024 Research Infrastucture is funded by the European Union's Horizon 2020 research and innovation programme under grant agreement No 871149.\n

\n\n\n

\n \n\n \n \n \n \n \n \n Landforms analysis of a Floor-Fractured Crater in Terra Sirenum, Mars.\n \n \n \n \n\n\n \n Bertoli, S.; Massironi, M.; Salvatore, M. C.; and Baroni, C.\n\n\n \n\n\n\n , 44: 387. July 2022.\n ADS Bibcode: 2022cosp...44..387B\n\n\n\n
\n\n\n\n \n \n $\"Landforms$ 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{bertoli_landforms_2022,\n\ttitle = {Landforms analysis of a {Floor}-{Fractured} {Crater} in {Terra} {Sirenum}, {Mars}},\n\tvolume = {44},\n\turl = {https://ui.adsabs.harvard.edu/abs/2022cosp...44..387B},\n\tabstract = {Floor-Fractured Craters (FFCs) are characterized by their typical floors, which exhibit fractures, mesas and knobs and they are found on different planetary bodies. The origin of fracturing is explained by many models that hypothesize different genesis. The periglacial one [1], considers the melting of subsurface ice reservoirs according to overburden material, resulting in increased temperature and pressure. In the model of groundwater migration [2], a confined aquifer and flowing water in the subsurface is needed. The water will lead to seepage and piping in the deposited crater filling. In the case of ice-rich subsurface, outflow could even form by tectonic pressurization [3]. Craters that are located close to volcanic areas on Mars could have a volcanic origin. Impacts lead to a reduction of crustal thickness beneath the crater, and magma could rise through this zone of weakness [4]. Another model has proposed a piecemeal caldera collapse [5]. So, it is indeed likely that diverse FFCs have different and, in some cases concurrent, genetic origins. Hence, it is extremely important to discriminate the geological features within FFCs for understanding their diverse evolution, which might or might not imply a relevant role of water. In this work, we focused on the analysis of the landforms of a Floor-Fractured Crater located in the southern hemisphere of Mars (37 ° S, 190 ° E) in Terra Sirenum. The crater, placed in the Gorgonian Chaos (a basin extended for about 240 km in diameter [6]) is about 18 km in diameter, has a smooth and degraded rim and a chaotic floor characterized by a polygonal fault network bounding large and irregular blocks. Through remote sensing, we analyzed different images at various spatial resolutions from the Mars Reconnaissance Orbiter (MRO) and of Mars Orbiter Laser Altimeter (MOLA) altimetric data. The photo-interpretative analysis led to compile a geomorphological map at the scale of 1:25,000 of the studied area in which we identified different Photogeological Units, i.e. areas that have the same characteristics of tone, texture, structure and response to erosion, as well as several landforms through landscape analysis. The recognized landforms have been classified according to their presumed morphogenesis, through a comparison, where possible, with terrestrial analogues. We suggest that the crater was modeled and modified by the action of at least three main morphogenetic agents: subsurface ice, gravity and wind, which interacted for remolding the structure of the crater floor dissected into several blocks by fractures and faults. Each block is characterized by a part of outcropping bedrock and slopes covered with debris and Latitude Dependent Mantle (LDM, [7]) in evident degradation state. In some cases, the blocks' slopes show evidence of wide gravitational collapses recalling deep-seated gravitational slope deformation (DSGSDs). Frequent periglacial forms, such as block fields, Pingo-like fields and polygonal terrain point towards a relevant presence of ice in the subsoil. This ice could indeed explain the formation of the chaotic floor of the area. In fact, referring to the model [1], the fracturing of the crater floor could be linked to the melting of a subsurface layer of ice, potentially due to the pressure of the overlying material. Usually, this model explains the very large chaotic terrains and a critical mass is needed to bring total melting of the underground ice. In our case (a crater of about 18 km in diameter), the filling material could have led only partial melting of the ice layer. Then the melting of ice stored in the pre-existing fractures, would have caused an underground runoff and the erosion of the fine materials within the fractured floor, possibly inducing DSGSDs at the blocks and crater margins. Acknowledgements. We would thank the Advanced Master on "GIScience and Unmanned System for the integrated management of the territory and the natural resources" of the University of Padua, in which this work was carried out and GMAP-EPN2024 and its Geology and Planetary Mapping winter School, organized in the frame of the European Union Horizon 2020 research and innovation program under grant agreements N. 871149. References. [1] Schumacher S., Zegers T. E. (2011) Icarus, V. 211, pp 305-315. [2] Sato H., Kurita K., Baratoux D. (2010), Icarus 207 pp. 248-264. [3] Hanna J. C., Phillips R. J. (2006) J. Geophys. Res., V. 111. [4] Bamberg M., Jaumann R., Asche H., Kneissl T., Michael G.G. (2014) Planetary and Space Science 98, pp.146-162. [5] Luzzi et al. (2021), Geophysical Resource Letters, V. 48. [6] Wendt L., Bishop J. L., Neukum G. (2013) Icarus 225, pp 200-215. [7] Kreslavsky, M. A., and J. W. Head. (2000). J. Geophys. Res., V. 105, pp. 26,695-26,712.},\n\turldate = {2023-02-25},\n\tauthor = {Bertoli, Silvia and Massironi, Matteo and Salvatore, Maria Cristina and Baroni, Carlo},\n\tmonth = jul,\n\tyear = {2022},\n\tnote = {ADS Bibcode: 2022cosp...44..387B},\n\tpages = {387},\n}\n\n

\n\n\n

\n Floor-Fractured Craters (FFCs) are characterized by their typical floors, which exhibit fractures, mesas and knobs and they are found on different planetary bodies. The origin of fracturing is explained by many models that hypothesize different genesis. The periglacial one [1], considers the melting of subsurface ice reservoirs according to overburden material, resulting in increased temperature and pressure. In the model of groundwater migration [2], a confined aquifer and flowing water in the subsurface is needed. The water will lead to seepage and piping in the deposited crater filling. In the case of ice-rich subsurface, outflow could even form by tectonic pressurization [3]. Craters that are located close to volcanic areas on Mars could have a volcanic origin. Impacts lead to a reduction of crustal thickness beneath the crater, and magma could rise through this zone of weakness [4]. Another model has proposed a piecemeal caldera collapse [5]. So, it is indeed likely that diverse FFCs have different and, in some cases concurrent, genetic origins. Hence, it is extremely important to discriminate the geological features within FFCs for understanding their diverse evolution, which might or might not imply a relevant role of water. In this work, we focused on the analysis of the landforms of a Floor-Fractured Crater located in the southern hemisphere of Mars (37 ° S, 190 ° E) in Terra Sirenum. The crater, placed in the Gorgonian Chaos (a basin extended for about 240 km in diameter [6]) is about 18 km in diameter, has a smooth and degraded rim and a chaotic floor characterized by a polygonal fault network bounding large and irregular blocks. Through remote sensing, we analyzed different images at various spatial resolutions from the Mars Reconnaissance Orbiter (MRO) and of Mars Orbiter Laser Altimeter (MOLA) altimetric data. The photo-interpretative analysis led to compile a geomorphological map at the scale of 1:25,000 of the studied area in which we identified different Photogeological Units, i.e. areas that have the same characteristics of tone, texture, structure and response to erosion, as well as several landforms through landscape analysis. The recognized landforms have been classified according to their presumed morphogenesis, through a comparison, where possible, with terrestrial analogues. We suggest that the crater was modeled and modified by the action of at least three main morphogenetic agents: subsurface ice, gravity and wind, which interacted for remolding the structure of the crater floor dissected into several blocks by fractures and faults. Each block is characterized by a part of outcropping bedrock and slopes covered with debris and Latitude Dependent Mantle (LDM, [7]) in evident degradation state. In some cases, the blocks' slopes show evidence of wide gravitational collapses recalling deep-seated gravitational slope deformation (DSGSDs). Frequent periglacial forms, such as block fields, Pingo-like fields and polygonal terrain point towards a relevant presence of ice in the subsoil. This ice could indeed explain the formation of the chaotic floor of the area. In fact, referring to the model [1], the fracturing of the crater floor could be linked to the melting of a subsurface layer of ice, potentially due to the pressure of the overlying material. Usually, this model explains the very large chaotic terrains and a critical mass is needed to bring total melting of the underground ice. In our case (a crater of about 18 km in diameter), the filling material could have led only partial melting of the ice layer. Then the melting of ice stored in the pre-existing fractures, would have caused an underground runoff and the erosion of the fine materials within the fractured floor, possibly inducing DSGSDs at the blocks and crater margins. Acknowledgements. We would thank the Advanced Master on \"GIScience and Unmanned System for the integrated management of the territory and the natural resources\" of the University of Padua, in which this work was carried out and GMAP-EPN2024 and its Geology and Planetary Mapping winter School, organized in the frame of the European Union Horizon 2020 research and innovation program under grant agreements N. 871149. References. [1] Schumacher S., Zegers T. E. (2011) Icarus, V. 211, pp 305-315. [2] Sato H., Kurita K., Baratoux D. (2010), Icarus 207 pp. 248-264. [3] Hanna J. C., Phillips R. J. (2006) J. Geophys. Res., V. 111. [4] Bamberg M., Jaumann R., Asche H., Kneissl T., Michael G.G. (2014) Planetary and Space Science 98, pp.146-162. [5] Luzzi et al. (2021), Geophysical Resource Letters, V. 48. [6] Wendt L., Bishop J. L., Neukum G. (2013) Icarus 225, pp 200-215. [7] Kreslavsky, M. A., and J. W. Head. (2000). J. Geophys. Res., V. 105, pp. 26,695-26,712.\n

\n\n\n

\n \n\n \n \n \n \n \n \n Automatic detection of bow shock and magnetopause boundaries at Mercury using MESSENGER magnetometer data.\n \n \n \n \n\n\n \n Nevskii, D.; Lavrukhin, A.; Julka, S.; Parunakian, D.; and Granitzer, M.\n\n\n \n\n\n\n , 44: 475. July 2022.\n ADS Bibcode: 2022cosp...44..475N\n\n\n\n
\n\n\n\n \n \n $\"Automatic$ 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{nevskii_automatic_2022,\n\ttitle = {Automatic detection of bow shock and magnetopause boundaries at {Mercury} using {MESSENGER} magnetometer data},\n\tvolume = {44},\n\turl = {https://ui.adsabs.harvard.edu/abs/2022cosp...44..475N},\n\tabstract = {The aim of this work is to develop methods for automatic processing of the MESSENGER (MErcury Surface, Space ENvironment, GEochemistry, and Ranging) spacecraft magnetometer data to search for the position of the bow shock and the magnetopause of the Mercury's magnetosphere. In our work we use different methods, including neural networks. In 2011 - 2015 MESSENGER spacecraft completed more than 4000 orbits around Mercury, thus giving data of more than 8000 crossings of bow shock as well as magnetopause of the planet. Given large data, Neural Networks can be expected to approximate complex functions, which often surpass deterministic and rule-based methods, in a variety of time series tasks like classification, time series forecasting and rare time series event detection. We leverage these to develop a predictor, that can be used in real-time during orbit, to predict magnetic region for each step in a short window of observation. The dataset was manually labelled with the boundary crossings. To supplement these, we also used the boundaries marked by Philpott et., al [1] for a few orbits. The windowed features are fed first into a block of 3 Convolutional layers with 1D filters, each followed by Batch Normalisation and ReLu activations. The activations obtained at the end of the CNN block are then passed to the Recurrent block with two layers of LSTMs. The final activations are then passed to a fully connected layer with softmax activations. The objective function used for training is Categorial cross entropy, with Adam optimizer. Also we have used other different methods for detecting the features associated with bow shock and magnetopause crossings. The search for extremum points is carried out using the RobustStatDetector method, which is part of the Kats library for time series analysis. This module smoothes the time series using a moving average, calculates the difference of the smoothed time series, gives the given parameter the number of calculated points, the standardized score and p-values for the calculated differences. The result of the method is a set of points in which the p-value is less than the set threshold parameter. The choice of this detection algorithm is due, among other things, to its selection of several extremum points in one run over the data volume. This work is carried out under the European Union's Horizon 2020 research and innovation programme under grant agreement No 871149. This work is carried out under RFBR grant no 21-52-12025. [1] L. C. Philpott et al. "The Shape of Mercury's Magnetopause: The Picture From MESSENGER Magnetometer Observations and Future Prospects for BepiColombo". In: Journal of Geophysical Research: Space Physics 125.5 (May 2020). issn: 2169-9380, 2169-9402. doi: 10.1029/2019JA027544.},\n\turldate = {2023-02-25},\n\tauthor = {Nevskii, Dmitrii and Lavrukhin, Alexander and Julka, Sahib and Parunakian, David and Granitzer, Michael},\n\tmonth = jul,\n\tyear = {2022},\n\tnote = {ADS Bibcode: 2022cosp...44..475N},\n\tpages = {475},\n}\n\n

\n\n\n

\n The aim of this work is to develop methods for automatic processing of the MESSENGER (MErcury Surface, Space ENvironment, GEochemistry, and Ranging) spacecraft magnetometer data to search for the position of the bow shock and the magnetopause of the Mercury's magnetosphere. In our work we use different methods, including neural networks. In 2011 - 2015 MESSENGER spacecraft completed more than 4000 orbits around Mercury, thus giving data of more than 8000 crossings of bow shock as well as magnetopause of the planet. Given large data, Neural Networks can be expected to approximate complex functions, which often surpass deterministic and rule-based methods, in a variety of time series tasks like classification, time series forecasting and rare time series event detection. We leverage these to develop a predictor, that can be used in real-time during orbit, to predict magnetic region for each step in a short window of observation. The dataset was manually labelled with the boundary crossings. To supplement these, we also used the boundaries marked by Philpott et., al [1] for a few orbits. The windowed features are fed first into a block of 3 Convolutional layers with 1D filters, each followed by Batch Normalisation and ReLu activations. The activations obtained at the end of the CNN block are then passed to the Recurrent block with two layers of LSTMs. The final activations are then passed to a fully connected layer with softmax activations. The objective function used for training is Categorial cross entropy, with Adam optimizer. Also we have used other different methods for detecting the features associated with bow shock and magnetopause crossings. The search for extremum points is carried out using the RobustStatDetector method, which is part of the Kats library for time series analysis. This module smoothes the time series using a moving average, calculates the difference of the smoothed time series, gives the given parameter the number of calculated points, the standardized score and p-values for the calculated differences. The result of the method is a set of points in which the p-value is less than the set threshold parameter. The choice of this detection algorithm is due, among other things, to its selection of several extremum points in one run over the data volume. This work is carried out under the European Union's Horizon 2020 research and innovation programme under grant agreement No 871149. This work is carried out under RFBR grant no 21-52-12025. [1] L. C. Philpott et al. \"The Shape of Mercury's Magnetopause: The Picture From MESSENGER Magnetometer Observations and Future Prospects for BepiColombo\". In: Journal of Geophysical Research: Space Physics 125.5 (May 2020). issn: 2169-9380, 2169-9402. doi: 10.1029/2019JA027544.\n

\n\n\n

\n \n\n \n \n \n \n \n \n Sun Planet Interactions Digital Environment on Request (SPIDER) for Europlanet RI H2024.\n \n \n \n \n\n\n \n Andre, N.\n\n\n \n\n\n\n , 44: 3468. July 2022.\n ADS Bibcode: 2022cosp...44.3468A\n\n\n\n
\n\n\n\n \n \n $\"Sun$ 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{andre_sun_2022,\n\ttitle = {Sun {Planet} {Interactions} {Digital} {Environment} on {Request} ({SPIDER}) for {Europlanet} {RI} {H2024}},\n\tvolume = {44},\n\turl = {https://ui.adsabs.harvard.edu/abs/2022cosp...44.3468A},\n\tabstract = {The H2020 Europlanet-2020 programme, which ended on Aug 31st, 2019, included an activity called PSWS (Planetary Space Weather Services), which provided 12 services distributed over four different domains (A. Prediction, B. Detection, C. Modelling, D. Alerts) and accessed through the PSWS portal (http://planetaryspaceweather-europlanet.irap.omp.eu/): A1. 1D MHD Solar Wind Prediction Tool - HELIOPROPA, A2. Propagation Tool, A3. Meteor showers, A4. Cometary tail crossings - TAILCATCHER, B1. Lunar impacts - ALFIE, B2. Giant planet fireballs - DeTeCt3.1, B3. Cometary tails - WINDSOCKS, C1. Earth, Mars, Venus, Jupiter coupling- TRANSPLANET, C2. Mars radiation environment - RADMAREE, C3. Giant planet magnetodiscs - MAGNETODISC, C4. Jupiter's thermosphere, D. Alerts. In the framework of the starting Europlanet-2024 programme, SPIDER will extend PSWS domains (A. Prediction, C. Modelling, E. Databases) services and give the European planetary scientists, space agencies and industries access to 6 unique, publicly available and sophisticated services in order to model planetary environments and solar wind interactions through the deployment of a dedicated run on request infrastructure and associated databases. C5. A service for runs on request of models of Jupiter's moon exospheres as well as the exosphere of Mercury, C6. A service to connect the open-source Spacecraft-Plasma Interaction Software (SPIS) software with models of space environments in order to compute the effect of spacecraft potential on scientific instruments onboard space missions. Pre-configured simulations will be made for Bepi-Colombo and JUICE missions, C7. A service for runs on request of particle tracing models in planetary magnetospheres, E1. A database of the high-energy particle flux proxy at Mars, Venus and comet 67P using background counts observed in the data obtained by the plasma instruments onboard Mars Express (operational from 2003), Venus Express (2006-2014), and Rosetta (2014-2015); E2. A simulation database for Mercury and Jupiter's moons magnetospheres and link them with prediction of the solar wind parameters from Europlanet-RI H2020 PSWS services. A1. An extension of the Europlanet-RI H2020 PSWS Heliopropa service in order to ingest new observations from Solar missions like the ESA Solar Orbiter or NASA Solar Parker Probe missions and use them as input parameters for solar wind prediction; These developments will be discussed in the presentation. The Europlanet 2020 Research Infrastructure project has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement No 654208. The Europlanet 2024 Research Infrastructure project has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement No 871149.},\n\turldate = {2023-02-25},\n\tauthor = {Andre, Nicolas},\n\tmonth = jul,\n\tyear = {2022},\n\tnote = {ADS Bibcode: 2022cosp...44.3468A},\n\tpages = {3468},\n}\n\n

\n\n\n

\n The H2020 Europlanet-2020 programme, which ended on Aug 31st, 2019, included an activity called PSWS (Planetary Space Weather Services), which provided 12 services distributed over four different domains (A. Prediction, B. Detection, C. Modelling, D. Alerts) and accessed through the PSWS portal (http://planetaryspaceweather-europlanet.irap.omp.eu/): A1. 1D MHD Solar Wind Prediction Tool - HELIOPROPA, A2. Propagation Tool, A3. Meteor showers, A4. Cometary tail crossings - TAILCATCHER, B1. Lunar impacts - ALFIE, B2. Giant planet fireballs - DeTeCt3.1, B3. Cometary tails - WINDSOCKS, C1. Earth, Mars, Venus, Jupiter coupling- TRANSPLANET, C2. Mars radiation environment - RADMAREE, C3. Giant planet magnetodiscs - MAGNETODISC, C4. Jupiter's thermosphere, D. Alerts. In the framework of the starting Europlanet-2024 programme, SPIDER will extend PSWS domains (A. Prediction, C. Modelling, E. Databases) services and give the European planetary scientists, space agencies and industries access to 6 unique, publicly available and sophisticated services in order to model planetary environments and solar wind interactions through the deployment of a dedicated run on request infrastructure and associated databases. C5. A service for runs on request of models of Jupiter's moon exospheres as well as the exosphere of Mercury, C6. A service to connect the open-source Spacecraft-Plasma Interaction Software (SPIS) software with models of space environments in order to compute the effect of spacecraft potential on scientific instruments onboard space missions. Pre-configured simulations will be made for Bepi-Colombo and JUICE missions, C7. A service for runs on request of particle tracing models in planetary magnetospheres, E1. A database of the high-energy particle flux proxy at Mars, Venus and comet 67P using background counts observed in the data obtained by the plasma instruments onboard Mars Express (operational from 2003), Venus Express (2006-2014), and Rosetta (2014-2015); E2. A simulation database for Mercury and Jupiter's moons magnetospheres and link them with prediction of the solar wind parameters from Europlanet-RI H2020 PSWS services. A1. An extension of the Europlanet-RI H2020 PSWS Heliopropa service in order to ingest new observations from Solar missions like the ESA Solar Orbiter or NASA Solar Parker Probe missions and use them as input parameters for solar wind prediction; These developments will be discussed in the presentation. The Europlanet 2020 Research Infrastructure project has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement No 654208. The Europlanet 2024 Research Infrastructure project has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement No 871149.\n

\n\n\n

\n \n\n \n \n \n \n \n \n Activities at a European Planetary Simulation Facility.\n \n \n \n \n\n\n \n Merrison, J.; Iversen, J. J.; Rasmussen, K.; and Waza, A.\n\n\n \n\n\n\n Technical Report EPSC2022-122, Copernicus Meetings, July 2022.\n \n\n\n\n
\n\n\n\n \n \n $\"Activities$ 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

@techreport{merrison_activities_2022,\n\ttitle = {Activities at a {European} {Planetary} {Simulation} {Facility}},\n\turl = {https://meetingorganizer.copernicus.org/EPSC2022/EPSC2022-122.html},\n\tlanguage = {en},\n\tnumber = {EPSC2022-122},\n\turldate = {2023-02-25},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Merrison, Jonathan and Iversen, Jens Jacob and Rasmussen, Keld and Waza, Andebo},\n\tmonth = jul,\n\tyear = {2022},\n\tdoi = {10.5194/epsc2022-122},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n In-situ measurement and sampling of Martian analogues in the Rio Tinto area in support of the Ma_MISS scientific activity.\n \n \n \n \n\n\n \n Ferrari, M.; Angelis, S. D.; Frigeri, A.; Sanctis, M. C. D.; Altieri, F.; Gomez, F.; Ammannito, E.; Costa, N.; Rossi, L.; and Formisano, M.\n\n\n \n\n\n\n Technical Report EPSC2022-153, Copernicus Meetings, July 2022.\n \n\n\n\n
\n\n\n\n \n \n $\"In-situ$ 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

@techreport{ferrari_-situ_2022,\n\ttitle = {In-situ measurement and sampling of {Martian} analogues in the {Rio} {Tinto} area in support of the {Ma}\\_MISS scientific activity},\n\turl = {https://meetingorganizer.copernicus.org/EPSC2022/EPSC2022-153.html},\n\tlanguage = {en},\n\tnumber = {EPSC2022-153},\n\turldate = {2023-02-25},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Ferrari, Marco and Angelis, Simone De and Frigeri, Alessandro and Sanctis, Maria Cristina De and Altieri, Francesca and Gomez, Felipe and Ammannito, Eleonora and Costa, Nicole and Rossi, Lorenzo and Formisano, Michelangelo},\n\tmonth = jul,\n\tyear = {2022},\n\tdoi = {10.5194/epsc2022-153},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Compositional and subsurface analysis of an outcrop close to Olympia Planum on Mars.\n \n \n \n \n\n\n \n Costa, N.; Massironi, M.; Penasa, L.; Nava, J.; Pozzobon, R.; and Ferrari, S.\n\n\n \n\n\n\n Technical Report EPSC2022-167, Copernicus Meetings, July 2022.\n \n\n\n\n
\n\n\n\n \n \n $\"Compositional$ 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

@techreport{costa_compositional_2022,\n\ttitle = {Compositional and subsurface analysis of an outcrop close to {Olympia} {Planum} on {Mars}},\n\turl = {https://meetingorganizer.copernicus.org/EPSC2022/EPSC2022-167.html},\n\tlanguage = {en},\n\tnumber = {EPSC2022-167},\n\turldate = {2023-02-25},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Costa, Nicole and Massironi, Matteo and Penasa, Luca and Nava, Jacopo and Pozzobon, Riccardo and Ferrari, Sabrina},\n\tmonth = jul,\n\tyear = {2022},\n\tdoi = {10.5194/epsc2022-167},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n The scenic tour of the Venusian subsolar magnetosheath by BepiColombo.\n \n \n \n \n\n\n \n Persson, M.\n\n\n \n\n\n\n Technical Report EPSC2022-397, Copernicus Meetings, July 2022.\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 1 download\n \n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@techreport{persson_scenic_2022,\n\ttitle = {The scenic tour of the {Venusian} subsolar magnetosheath by {BepiColombo}},\n\turl = {https://meetingorganizer.copernicus.org/EPSC2022/EPSC2022-397.html},\n\tlanguage = {en},\n\tnumber = {EPSC2022-397},\n\turldate = {2023-02-25},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Persson, Moa},\n\tmonth = jul,\n\tyear = {2022},\n\tdoi = {10.5194/epsc2022-397},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n JSON Implementation of Time-Frequency Radio Catalogues: TFCat.\n \n \n \n \n\n\n \n Cecconi, B.; Bonnin, X.; Loh, A.; Louis, C.; and Taylor, M.\n\n\n \n\n\n\n Technical Report EPSC2022-426, Copernicus Meetings, July 2022.\n \n\n\n\n
\n\n\n\n \n \n $\"JSON$ 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

@techreport{cecconi_json_2022,\n\ttitle = {{JSON} {Implementation} of {Time}-{Frequency} {Radio} {Catalogues}: {TFCat}},\n\tshorttitle = {{JSON} {Implementation} of {Time}-{Frequency} {Radio} {Catalogues}},\n\turl = {https://meetingorganizer.copernicus.org/EPSC2022/EPSC2022-426.html},\n\tlanguage = {en},\n\tnumber = {EPSC2022-426},\n\turldate = {2023-02-25},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Cecconi, Baptiste and Bonnin, Xavier and Loh, Alan and Louis, Corentin and Taylor, Mark},\n\tmonth = jul,\n\tyear = {2022},\n\tdoi = {10.5194/epsc2022-426},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n A dual approach for the successful dissemination, use and improvement of educational resources in planetary science.\n \n \n \n \n\n\n \n Segade, U. P.; Heward, A.; and Duras, F.\n\n\n \n\n\n\n Technical Report EPSC2022-491, Copernicus Meetings, July 2022.\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

@techreport{segade_dual_2022,\n\ttitle = {A dual approach for the successful dissemination, use and improvement of educational resources in planetary science.},\n\turl = {https://meetingorganizer.copernicus.org/EPSC2022/EPSC2022-491.html},\n\tlanguage = {en},\n\tnumber = {EPSC2022-491},\n\turldate = {2023-02-25},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Segade, Ulysse Pedreira and Heward, Anita and Duras, Federica},\n\tmonth = jul,\n\tyear = {2022},\n\tdoi = {10.5194/epsc2022-491},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Volumetric changes of mud on Mars: Evidence from laboratory simulations.\n \n \n \n \n\n\n \n Brož, P.; Kryza, O.; Conway, S.; Mazzini, A.; Hauber, E.; Sylvest, M.; and Patel, M.\n\n\n \n\n\n\n Technical Report EPSC2022-548, Copernicus Meetings, July 2022.\n \n\n\n\n
\n\n\n\n \n \n $\"Volumetric$ 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

@techreport{broz_volumetric_2022,\n\ttitle = {Volumetric changes of mud on {Mars}: {Evidence} from laboratory simulations},\n\tshorttitle = {Volumetric changes of mud on {Mars}},\n\turl = {https://meetingorganizer.copernicus.org/EPSC2022/EPSC2022-548.html},\n\tlanguage = {en},\n\tnumber = {EPSC2022-548},\n\turldate = {2023-02-25},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Brož, Petr and Kryza, Ondrej and Conway, Susan and Mazzini, Adriano and Hauber, Ernst and Sylvest, Matthew and Patel, Manish},\n\tmonth = jul,\n\tyear = {2022},\n\tdoi = {10.5194/epsc2022-548},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Educational Resources for EPN24 Planetary Field Analogue Sites.\n \n \n \n \n\n\n \n Thompson, T.; and Cane, R.\n\n\n \n\n\n\n Technical Report EPSC2022-612, Copernicus Meetings, July 2022.\n \n\n\n\n
\n\n\n\n \n \n $\"Educational$ 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

@techreport{thompson_educational_2022,\n\ttitle = {Educational {Resources} for {EPN24} {Planetary} {Field} {Analogue} {Sites}},\n\turl = {https://meetingorganizer.copernicus.org/EPSC2022/EPSC2022-612.html},\n\tlanguage = {en},\n\tnumber = {EPSC2022-612},\n\turldate = {2023-02-25},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Thompson, Tony and Cane, Rosie},\n\tmonth = jul,\n\tyear = {2022},\n\tdoi = {10.5194/epsc2022-612},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Spectral properties of the lunar Tsiolkovskiy crater through Spectral Units identification and analysis.\n \n \n \n \n\n\n \n Tognon, G.; Zambon, F.; Carli, C.; and Massironi, M.\n\n\n \n\n\n\n Technical Report EPSC2022-622, Copernicus Meetings, July 2022.\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\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@techreport{tognon_spectral_2022,\n\ttitle = {Spectral properties of the lunar {Tsiolkovskiy} crater through {Spectral} {Units} identification and analysis},\n\turl = {https://meetingorganizer.copernicus.org/EPSC2022/EPSC2022-622.html},\n\tlanguage = {en},\n\tnumber = {EPSC2022-622},\n\turldate = {2023-02-25},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Tognon, Gloria and Zambon, Francesca and Carli, Cristian and Massironi, Matteo},\n\tmonth = jul,\n\tyear = {2022},\n\tdoi = {10.5194/epsc2022-622},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Mentorship opportunities.\n \n \n \n \n\n\n \n Stonkute, E.\n\n\n \n\n\n\n Technical Report EPSC2022-780, Copernicus Meetings, July 2022.\n \n\n\n\n
\n\n\n\n \n \n $\"Mentorship$ 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

@techreport{stonkute_mentorship_2022,\n\ttitle = {Mentorship opportunities},\n\turl = {https://meetingorganizer.copernicus.org/EPSC2022/EPSC2022-780.html},\n\tlanguage = {en},\n\tnumber = {EPSC2022-780},\n\turldate = {2023-02-25},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Stonkute, Edita},\n\tmonth = jul,\n\tyear = {2022},\n\tdoi = {10.5194/epsc2022-780},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n The Effect of the Solid Phase Adopted by Astrophysical Ices on their Radiation Chemistry and Physics: Implications for the Synthesis of Prebiotic Molecules.\n \n \n \n \n\n\n \n Mifsud, D.; Hailey, P.; Herczku, P.; Juhász, Z.; Kovács, S.; Sulik, B.; Kushwaha, R. K.; Rácz, R.; Biri, S.; Ioppolo, S.; Kaňuchová, Z.; Paripás, B.; McCullough, R.; and Mason, N.\n\n\n \n\n\n\n Technical Report EPSC2022-832, Copernicus Meetings, July 2022.\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

@techreport{mifsud_effect_2022,\n\ttitle = {The {Effect} of the {Solid} {Phase} {Adopted} by {Astrophysical} {Ices} on their {Radiation} {Chemistry} and {Physics}: {Implications} for the {Synthesis} of {Prebiotic} {Molecules}},\n\tshorttitle = {The {Effect} of the {Solid} {Phase} {Adopted} by {Astrophysical} {Ices} on their {Radiation} {Chemistry} and {Physics}},\n\turl = {https://meetingorganizer.copernicus.org/EPSC2022/EPSC2022-832.html},\n\tlanguage = {en},\n\tnumber = {EPSC2022-832},\n\turldate = {2023-02-25},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Mifsud, Duncan and Hailey, Perry and Herczku, Péter and Juhász, Zoltán and Kovács, Sándor and Sulik, Béla and Kushwaha, Rahul Kumar and Rácz, Richard and Biri, Sándor and Ioppolo, Sergio and Kaňuchová, Zuzana and Paripás, Béla and McCullough, Robert and Mason, Nigel},\n\tmonth = jul,\n\tyear = {2022},\n\tdoi = {10.5194/epsc2022-832},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Unravelling icy Planetary Surfaces: Insights on their tectonic DEformation from field Survey - UPSIDES.\n \n \n \n \n\n\n \n Rossi, C.; Cianfarra, P.; Lucchetti, A.; Pozzobon, R.; Penasa, L.; Munaretto, G.; and Pajola, M.\n\n\n \n\n\n\n Technical Report EPSC2022-874, Copernicus Meetings, July 2022.\n \n\n\n\n
\n\n\n\n \n \n $\"Unravelling$ 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

@techreport{rossi_unravelling_2022,\n\ttitle = {Unravelling icy {Planetary} {Surfaces}: {Insights} on their tectonic {DEformation} from field {Survey} - {UPSIDES}},\n\tshorttitle = {Unravelling icy {Planetary} {Surfaces}},\n\turl = {https://meetingorganizer.copernicus.org/EPSC2022/EPSC2022-874.html},\n\tlanguage = {en},\n\tnumber = {EPSC2022-874},\n\turldate = {2023-02-25},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Rossi, Costanza and Cianfarra, Paola and Lucchetti, Alice and Pozzobon, Riccardo and Penasa, Luca and Munaretto, Giovanni and Pajola, Maurizio},\n\tmonth = jul,\n\tyear = {2022},\n\tdoi = {10.5194/epsc2022-874},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Reference emission spectral data for astronomical observations.\n \n \n \n \n\n\n \n Orszagh, J.; Stachova, B.; Blasko, J.; Matejcik, S.; Bodewits, D.; and Bromley, S.\n\n\n \n\n\n\n Technical Report EPSC2022-950, Copernicus Meetings, July 2022.\n \n\n\n\n
\n\n\n\n \n \n $\"Reference$ 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

@techreport{orszagh_reference_2022,\n\ttitle = {Reference emission spectral data for astronomical observations},\n\turl = {https://meetingorganizer.copernicus.org/EPSC2022/EPSC2022-950.html},\n\tlanguage = {en},\n\tnumber = {EPSC2022-950},\n\turldate = {2023-02-25},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Orszagh, Juraj and Stachova, Barbora and Blasko, Jan and Matejcik, Stefan and Bodewits, Dennis and Bromley, Steven},\n\tmonth = jul,\n\tyear = {2022},\n\tdoi = {10.5194/epsc2022-950},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Morphometry of an hexagonal pit crater in Pavonis Mons, Mars.\n \n \n \n \n\n\n \n Nodjoumi, G.; Pozzobon, R.; Sauro, F.; and Rossi, A. P.\n\n\n \n\n\n\n Technical Report EPSC2022-1128, Copernicus Meetings, July 2022.\n \n\n\n\n
\n\n\n\n \n \n $\"Morphometry$ 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

@techreport{nodjoumi_morphometry_2022,\n\ttitle = {Morphometry of an hexagonal pit crater in {Pavonis} {Mons}, {Mars}},\n\turl = {https://meetingorganizer.copernicus.org/EPSC2022/EPSC2022-1128.html},\n\tlanguage = {en},\n\tnumber = {EPSC2022-1128},\n\turldate = {2023-02-25},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Nodjoumi, Giacomo and Pozzobon, Riccardo and Sauro, Francesco and Rossi, Angelo Pio},\n\tmonth = jul,\n\tyear = {2022},\n\tdoi = {10.5194/epsc2022-1128},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Participation Trends and Geographical Diversity in Earth and Space Science.\n \n \n \n \n\n\n \n Illyés, A.; Opitz, A.; and Heward, A.\n\n\n \n\n\n\n Technical Report EPSC2022-1168, Copernicus Meetings, July 2022.\n \n\n\n\n
\n\n\n\n \n \n $\"Participation$ 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 1 download\n \n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@techreport{illyes_participation_2022,\n\ttitle = {Participation {Trends} and {Geographical} {Diversity} in {Earth} and {Space} {Science}},\n\turl = {https://meetingorganizer.copernicus.org/EPSC2022/EPSC2022-1168.html},\n\tlanguage = {en},\n\tnumber = {EPSC2022-1168},\n\turldate = {2023-02-25},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Illyés, András and Opitz, Andrea and Heward, Anita},\n\tmonth = jul,\n\tyear = {2022},\n\tdoi = {10.5194/epsc2022-1168},\n}\n

\n\n\n\n

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

\n\n

\n \n 2021\n \n \n (23)\n \n \n

\n \n \n

\n \n\n \n \n \n \n \n \n Facilitating reuse of planetary spatial research data – Conceptualizing an open map repository as part of a Planetary Research Data Infrastructure.\n \n \n \n \n\n\n \n Nass, A.; Asch, K.; Van Gasselt, S.; Rossi, A. P.; Besse, S.; Cecconi, B.; Frigeri, A.; Hare, T.; Hargitai, H.; and Manaud, N.\n\n\n \n\n\n\n Planetary and Space Science, 204: 105269. September 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Facilitating$ 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{nass_facilitating_2021,\n\ttitle = {Facilitating reuse of planetary spatial research data – {Conceptualizing} an open map repository as part of a {Planetary} {Research} {Data} {Infrastructure}},\n\tvolume = {204},\n\tissn = {00320633},\n\turl = {https://linkinghub.elsevier.com/retrieve/pii/S0032063321001082},\n\tdoi = {10.1016/j.pss.2021.105269},\n\tlanguage = {en},\n\turldate = {2024-05-08},\n\tjournal = {Planetary and Space Science},\n\tauthor = {Nass, Andrea and Asch, Kristine and Van Gasselt, Stephan and Rossi, Angelo Pio and Besse, Sebastien and Cecconi, Baptiste and Frigeri, Alessandro and Hare, Trent and Hargitai, Henrik and Manaud, Nicolas},\n\tmonth = sep,\n\tyear = {2021},\n\tpages = {105269},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Machine Learning Pipeline for Automated Detection of ICMEs.\n \n \n \n \n\n\n \n Rüdisser, H.; and Amerstorfer, U.\n\n\n \n\n\n\n September 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Machine$ 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\n\n

@misc{rudisser_machine_2021,\n\taddress = {virtual},\n\ttype = {Workshop},\n\ttitle = {Machine {Learning} {Pipeline} for {Automated} {Detection} of {ICMEs}},\n\turl = {https://www.europlanet-society.org/wp-content/uploads/2024/02/296.pdf},\n\tabstract = {The work package “Machine Learning Solutions for Data Analysis and Exploitation in Planetary Science” within Europlanet 2024 Research Infrastructure will develop machine learning (ML) powered data analysis and exploitation tools optimized for planetary science.\nIn this workshop, held in the course of theEuroplanet Science Congress 2021, we will introduce an ML pipeline for the automated detection of interplanetary coronal mass ejections (ICMEs) in solar wind time series data. First, we will briefly give an overview about the physical problem and its relevance for space weather. Then, we will guide the participants through the developed ML code with the help of a sample data set of solar wind time series data from different spacecraft. At the end, we will also cover problems encountered during the development of the pipeline.\n\nThe code for the ML pipeline will be freely available on the repository “EPSC2021-ICME-workshop” of our public GitHub account. We strongly encourage the participants to clone the repository and have a look at the material prior to the workshop.\n\nEuroplanet 2024 RI has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No 871149.},\n\tlanguage = {English},\n\tauthor = {Rüdisser, H.T. and Amerstorfer, U.V.},\n\tmonth = sep,\n\tyear = {2021},\n\tkeywords = {workshop},\n}\n\n

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

\n\n\n

\n \n\n \n \n \n \n \n \n Machine Learning Pipeline for Automated Detection of Boundary Crossings around Mercury.\n \n \n \n \n\n\n \n Julka, S.; and Parunakian, D.\n\n\n \n\n\n\n September 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Machine$ 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\n\n

@misc{julka_machine_2021,\n\taddress = {virtual},\n\ttype = {Workshop},\n\ttitle = {Machine {Learning} {Pipeline} for {Automated} {Detection} of {Boundary} {Crossings} around {Mercury}},\n\turl = {https://www.europlanet-society.org/wp-content/uploads/2024/02/295-1.pdf},\n\tabstract = {The work package “Machine Learning Solutions for Data Analysis and Exploitation in Planetary Science” within Europlanet 2024 Research Infrastructure will develop machine learning (ML) powered data analysis and exploitation tools optimized for planetary science.\nIn this workshop, held in the course of theEuroplanet Science Congress 2021, we will introduce an ML pipeline for the automated detection of boundary crossings around Mercury in solar wind time series data. First, we will briefly give an overview about the physical problem. Then, we will guide the participants through the developed ML code with the help of a sample data set of solar wind time series data from the MESSENGER spacecraft. At the end, we will also cover problems encountered during the development of the pipeline.\n\nThe code for the ML pipeline will be freely available on the repository “EPSC2021-MercuryBoundaries-workshop” of our public GitHub account. We strongly encourage the participants to clone the repository and have a look at the material prior to the workshop.\n\nEuroplanet 2024 RI has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No 871149.},\n\tlanguage = {English},\n\tauthor = {Julka, S. and Parunakian, D.},\n\tmonth = sep,\n\tyear = {2021},\n\tkeywords = {workshop},\n}\n\n

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

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\n \n\n \n \n \n \n \n \n Determination of magnetopause and bow shock shape based on convolutional neural network modelling of MESSENGER data.\n \n \n \n \n\n\n \n Lavrukhin, A.; Parunakian, D.; Nevsky, D.; Julka, S.; Granitzer, M.; Windisch, A.; and Amerstorfer, U.\n\n\n \n\n\n\n Technical Report EPSC2021-651, EPSC 2021, September 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Determination$ 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

@techreport{lavrukhin_determination_2021,\n\ttype = {Conference presentation},\n\ttitle = {Determination of magnetopause and bow shock shape based on convolutional neural network modelling of {MESSENGER} data},\n\turl = {https://www.europlanet-society.org/wp-content/uploads/2024/02/268.pdf},\n\tabstract = {The magnetosphere of Mercury is relatively small and highly dynamic, mostly due to the weak planetary magnetic field. Varying solar wind conditions principally determine the location of both the Hermean bow shock and magnetopause. In 2011 – 2015 MESSENGER spacecraft completed over 4000 orbits around Mercury, thus giving a data of more than 8000 crossings of bow shock and magnetopause of the planet, this makes it possible to study in detail the bow shock, the magnetopause and the magnetosheath structures.\n\nIn this work we determine crossings of the bow shock and the magnetopause of Mercury by applying machine learning methods to the MESSENGER magnetometer data. We attempt to identify the crossings during the whole duration of the orbital mission and model the average three-dimensional shapes of these boundaries. The results are compared with those previously obtained in other works.\n\nThis work may be of interest for future Mercury research related to the BepiColombo spacecraft mission, which will enter the orbit around the planet in December 2025.},\n\tlanguage = {English},\n\tnumber = {EPSC2021-651},\n\tinstitution = {EPSC 2021},\n\tauthor = {Lavrukhin, A. and Parunakian, D. and Nevsky, D. and Julka, S. and Granitzer, M. and Windisch, A. and Amerstorfer, U.},\n\tmonth = sep,\n\tyear = {2021},\n}\n\n

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

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\n \n\n \n \n \n \n \n \n Automatic Detection and Classification of Boundary Crossings in Spacecraft in situ Data.\n \n \n \n \n\n\n \n Rüdisser, H.; Windisch, A.; Amerstorfer, U.; Soucek, J.; and Pisa, D.\n\n\n \n\n\n\n Technical Report P15C-2122, AGU Fall meeting 2021, December 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Automatic$ 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

@techreport{rudisser_automatic_2021,\n\ttype = {Conference presentation},\n\ttitle = {Automatic {Detection} and {Classification} of {Boundary} {Crossings} in {Spacecraft} in situ {Data}},\n\turl = {https://www.europlanet-society.org/wp-content/uploads/2024/02/255-1.pdf},\n\tabstract = {Planetary magnetospheres create multiple sharp boundaries, such as the bow shock, where the solar wind plasma is decelerated and compressed, or the magnetopause, a transition between solar wind field and planetary field. We attempt to use convolutional neural networks (CNNs) to identify magnetospheric boundaries, i.e. planetary and interplanetary shocks crossings and magnetopause crossings in spacecraft in situ data. The boundaries are identified by a discontinuity in a magnetic field, plasma density, and in the spectrum of high-frequency waves. These measurements are available on many planetary missions. Data from Earth’s missions Cluster and THEMIS are used for CNN training. We ultimately strive for successful classification of boundaries (shock, magnetopause, inbound, outbound) and the correct handling of multiple crossings.},\n\tlanguage = {English},\n\tnumber = {P15C-2122},\n\tinstitution = {AGU Fall meeting 2021},\n\tauthor = {Rüdisser, H. and Windisch, A. and Amerstorfer, U.V. and Soucek, J. and Pisa, D.},\n\tmonth = dec,\n\tyear = {2021},\n}\n\n

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\n \n\n \n \n \n \n \n \n Objective Geological and Geomorphological Mapping of 6. Martian Sedimentary Deposits: an Example From the Southeastern Margin of Holden Crater.\n \n \n \n \n\n\n \n Di Pietro, I.; Pondrelli, M.; Frigeri, A.; Marinangeli, L.; Tangari, A. C.; Pantaloni, M.; Luzzi, E.; Pozzobon, R.; Nass, A.; Massironi, M.; and Rossi, A. P.\n\n\n \n\n\n\n In September 2021. \n \n\n\n\n
\n\n\n\n \n \n $\"Objective$ 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

@inproceedings{di_pietro_objective_2021,\n\ttitle = {Objective {Geological} and {Geomorphological} {Mapping} of 6. {Martian} {Sedimentary} {Deposits}: an {Example} {From} the {Southeastern} {Margin} of {Holden} {Crater}},\n\turl = {https://www.europlanet-society.org/wp-content/uploads/2024/02/180.pdf},\n\tauthor = {Di Pietro, Ilaria and Pondrelli, Monica and Frigeri, Alessandro and Marinangeli, Lucia and Tangari, Anna Chiara and Pantaloni, Marco and Luzzi, Erica and Pozzobon, Riccardo and Nass, Andrea and Massironi, Matteo and Rossi, Angelo Pio},\n\tmonth = sep,\n\tyear = {2021},\n}\n\n

\n\n\n\n

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\n \n\n \n \n \n \n \n \n Interaction of Saturn’s Hexagon With Convective Storms.\n \n \n \n \n\n\n \n Sánchez‐Lavega, A.; García‐Melendo, E.; Del Río‐Gaztelurrutia, T.; Hueso, R.; Simon, A.; Wong, M. H.; Ahrens‐Velásquez, K.; Soria, M.; Barry, T.; Go, C.; and Foster, C.\n\n\n \n\n\n\n Geophysical Research Letters, 48(8): e2021GL092461. April 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Interaction$ 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{sanchezlavega_interaction_2021,\n\ttitle = {Interaction of {Saturn}’s {Hexagon} {With} {Convective} {Storms}},\n\tvolume = {48},\n\tissn = {0094-8276, 1944-8007},\n\turl = {https://agupubs.onlinelibrary.wiley.com/doi/10.1029/2021GL092461},\n\tdoi = {10.1029/2021GL092461},\n\tabstract = {Abstract\n            In March 2020, a convective storm erupted at planetographic latitude 76°N in the southern flank of Saturn’s long‐lived hexagonal wave. The storm reached a zonal size of 4,500 km and developed a tail extending zonally 33,000 km. Two new short‐lived storms erupted in May in the hexagon edge. These storms formed after the convective storms that took place in 2018 in nearby latitudes. There were no noticeable changes in the zonal profile of Saturn's polar winds in 2018–2020. Measurements of the longitude position of the vertices of the hexagon throughout this period yield a value for its period of rotation equal to that of System III of radio rotation measured at the time of Voyagers. We report changes in the hexagon clouds related to the activity of the storms. Our study reinforces the idea that Saturn’s hexagon is a well‐rooted structure with a possible direct relationship with the bulk rotation of the planet.\n          , \n            Plain Language Summary\n            Convective storms of zonal extents greater than 4,000 km are rare in Saturn's atmosphere. They occur every few years, and exceptionally (perhaps once every 20–30 years) they reach 10,000 km and become a Great White Spot that expands along an entire latitudinal band of the planet. In 2018, multiple eruptions of medium‐sized storms occurred close to the North Polar Region. After a period of calm throughout 2019, new eruptions took place in 2020 at 76°N latitude on the border of the hexagon wave, the closest to the pole ever observed. These storms changed the morphology of the clouds in the region, but the hexagon itself was not affected in its motion or dynamics, with no change in the zonal winds. This, together with its longevity, indicates that the hexagon is a robust meteorological formation. Its rotation period in these years remained that of the System III radio rotation measured by the Voyager spacecraft, reinforcing the idea of its possible direct relationship with the bulk rotation of the planet.\n          , \n            Key Points\n            \n              \n                \n                  Following an outbreak of polar storms in 2018, we observed in March–May 2020 a new episode of storms south of Saturn's hexagonal wave\n                \n                \n                  The storms did not produce a noticeable change in the zonal wind profile in the polar area\n                \n                \n                  The hexagon shape was perturbed after the storms but the wave suffered no change in its rotation period matching that of System III},\n\tlanguage = {en},\n\tnumber = {8},\n\turldate = {2023-12-21},\n\tjournal = {Geophysical Research Letters},\n\tauthor = {Sánchez‐Lavega, A. and García‐Melendo, E. and Del Río‐Gaztelurrutia, T. and Hueso, R. and Simon, A. and Wong, M. H. and Ahrens‐Velásquez, K. and Soria, M. and Barry, T. and Go, C. and Foster, C.},\n\tmonth = apr,\n\tyear = {2021},\n\tpages = {e2021GL092461},\n}\n\n

\n\n\n

\n Abstract In March 2020, a convective storm erupted at planetographic latitude 76°N in the southern flank of Saturn’s long‐lived hexagonal wave. The storm reached a zonal size of 4,500 km and developed a tail extending zonally 33,000 km. Two new short‐lived storms erupted in May in the hexagon edge. These storms formed after the convective storms that took place in 2018 in nearby latitudes. There were no noticeable changes in the zonal profile of Saturn's polar winds in 2018–2020. Measurements of the longitude position of the vertices of the hexagon throughout this period yield a value for its period of rotation equal to that of System III of radio rotation measured at the time of Voyagers. We report changes in the hexagon clouds related to the activity of the storms. Our study reinforces the idea that Saturn’s hexagon is a well‐rooted structure with a possible direct relationship with the bulk rotation of the planet. , Plain Language Summary Convective storms of zonal extents greater than 4,000 km are rare in Saturn's atmosphere. They occur every few years, and exceptionally (perhaps once every 20–30 years) they reach 10,000 km and become a Great White Spot that expands along an entire latitudinal band of the planet. In 2018, multiple eruptions of medium‐sized storms occurred close to the North Polar Region. After a period of calm throughout 2019, new eruptions took place in 2020 at 76°N latitude on the border of the hexagon wave, the closest to the pole ever observed. These storms changed the morphology of the clouds in the region, but the hexagon itself was not affected in its motion or dynamics, with no change in the zonal winds. This, together with its longevity, indicates that the hexagon is a robust meteorological formation. Its rotation period in these years remained that of the System III radio rotation measured by the Voyager spacecraft, reinforcing the idea of its possible direct relationship with the bulk rotation of the planet. , Key Points Following an outbreak of polar storms in 2018, we observed in March–May 2020 a new episode of storms south of Saturn's hexagonal wave The storms did not produce a noticeable change in the zonal wind profile in the polar area The hexagon shape was perturbed after the storms but the wave suffered no change in its rotation period matching that of System III\n

\n\n\n

\n \n\n \n \n \n \n \n \n Jupiter’s Great Red Spot: Strong Interactions With Incoming Anticyclones in 2019.\n \n \n \n \n\n\n \n Sánchez‐Lavega, A.; Anguiano‐Arteaga, A.; Iñurrigarro, P.; Garcia‐Melendo, E.; Legarreta, J.; Hueso, R.; Sanz‐Requena, J. F.; Pérez‐Hoyos, S.; Mendikoa, I.; Soria, M.; Rojas, J. F.; Andrés‐Carcasona, M.; Prat‐Gasull, A.; Ordoñez‐Extebarria, I.; Rogers, J. H.; Foster, C.; Mizumoto, S.; Casely, A.; Hansen, C. J.; Orton, G. S.; Momary, T.; and Eichstädt, G.\n\n\n \n\n\n\n Journal of Geophysical Research: Planets, 126(4): e2020JE006686. April 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Jupiter’s$ 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{sanchezlavega_jupiters_2021,\n\ttitle = {Jupiter’s {Great} {Red} {Spot}: {Strong} {Interactions} {With} {Incoming} {Anticyclones} in 2019},\n\tvolume = {126},\n\tissn = {2169-9097, 2169-9100},\n\tshorttitle = {Jupiter’s {Great} {Red} {Spot}},\n\turl = {https://agupubs.onlinelibrary.wiley.com/doi/10.1029/2020JE006686},\n\tdoi = {10.1029/2020JE006686},\n\tabstract = {Abstract\n            Jupiter’s Great Red Spot (GRS), a giant anticyclone, is the largest and longest‐lived of all the vortices observed in planetary atmospheres. During its history, the GRS has shrunk to half its size since 1879, and encountered many smaller anticyclones and other dynamical features that interacted in a complex way. In 2018–2020, while having a historically small size, its structure and even its survival appeared to be threatened when a series of anticyclones moving in from the east tore off large fragments of the red area and distorted its shape. In this work, we report observations of the dynamics of these interactions and show that as a result the GRS increased its internal rotation velocity, maintaining its vorticity but decreasing its visible area, and suffering a transient change in its otherwise steady 90‐day oscillation in longitude. From a radiative transfer analysis and numerical simulations of the dynamics we show that the interactions affected the upper cloud tops of the GRS. We argue that the intense vorticity of the GRS, together with its larger size and depth compared to the interacting vortices, guarantees its long lifetime.\n          , \n            Plain Language Summary\n            Jupiter’s Great Red Spot (GRS) is a giant anticyclone with a length that has shrunk since 1879 from ∼ 40,000 km to its current value of 15,000 km. The GRS is the longest‐lived of all the planetary vortices, observed perhaps since the 17th century. During its history, the GRS has encountered a variety of smaller anticyclones and other dynamical features, surviving these interactions. In 2018–2020, a series of anticyclones interacted with it, and tore off large fragments of its red area (called “flakes”), eroding and distorting its oval shape, and apparently threatening its survival. The interactions produced an increase in the GRS internal rotation velocity accompanied by a transient increase in the period and amplitude of its steady 90‐day oscillation in longitude. From the analysis of the reflectivity of the GRS and flakes and model simulations of the dynamics of the interactions we find that these events are likely to have been superficial, not affecting the full depth of the GRS. The interactions are not necessarily destructive but can transfer energy to the GRS, maintaining it in a steady state and guaranteeing its long lifetime.\n          , \n            Key Points\n            \n              \n                \n                  In 2018–2020, Jupiter’s Great Red Spot interacted with series of anticyclones, losing part of its visible red area and distorting its shape\n                \n                \n                  The Great Red Spot (GRS) increased its tangential velocity; it did not change its vorticity, but did temporarily change its 90‐day oscillation in longitude\n                \n                \n                  Dynamical and radiative transfer modeling shows that the interactions affected the upper cloud of the GRS with no risk for its survival},\n\tlanguage = {en},\n\tnumber = {4},\n\turldate = {2023-12-21},\n\tjournal = {Journal of Geophysical Research: Planets},\n\tauthor = {Sánchez‐Lavega, A. and Anguiano‐Arteaga, A. and Iñurrigarro, P. and Garcia‐Melendo, E. and Legarreta, J. and Hueso, R. and Sanz‐Requena, J. F. and Pérez‐Hoyos, S. and Mendikoa, I. and Soria, M. and Rojas, J. F. and Andrés‐Carcasona, M. and Prat‐Gasull, A. and Ordoñez‐Extebarria, I. and Rogers, J. H. and Foster, C. and Mizumoto, S. and Casely, A. and Hansen, C. J. and Orton, G. S. and Momary, T. and Eichstädt, G.},\n\tmonth = apr,\n\tyear = {2021},\n\tpages = {e2020JE006686},\n}\n\n

\n\n\n

\n Abstract Jupiter’s Great Red Spot (GRS), a giant anticyclone, is the largest and longest‐lived of all the vortices observed in planetary atmospheres. During its history, the GRS has shrunk to half its size since 1879, and encountered many smaller anticyclones and other dynamical features that interacted in a complex way. In 2018–2020, while having a historically small size, its structure and even its survival appeared to be threatened when a series of anticyclones moving in from the east tore off large fragments of the red area and distorted its shape. In this work, we report observations of the dynamics of these interactions and show that as a result the GRS increased its internal rotation velocity, maintaining its vorticity but decreasing its visible area, and suffering a transient change in its otherwise steady 90‐day oscillation in longitude. From a radiative transfer analysis and numerical simulations of the dynamics we show that the interactions affected the upper cloud tops of the GRS. We argue that the intense vorticity of the GRS, together with its larger size and depth compared to the interacting vortices, guarantees its long lifetime. , Plain Language Summary Jupiter’s Great Red Spot (GRS) is a giant anticyclone with a length that has shrunk since 1879 from ∼ 40,000 km to its current value of 15,000 km. The GRS is the longest‐lived of all the planetary vortices, observed perhaps since the 17th century. During its history, the GRS has encountered a variety of smaller anticyclones and other dynamical features, surviving these interactions. In 2018–2020, a series of anticyclones interacted with it, and tore off large fragments of its red area (called “flakes”), eroding and distorting its oval shape, and apparently threatening its survival. The interactions produced an increase in the GRS internal rotation velocity accompanied by a transient increase in the period and amplitude of its steady 90‐day oscillation in longitude. From the analysis of the reflectivity of the GRS and flakes and model simulations of the dynamics of the interactions we find that these events are likely to have been superficial, not affecting the full depth of the GRS. The interactions are not necessarily destructive but can transfer energy to the GRS, maintaining it in a steady state and guaranteeing its long lifetime. , Key Points In 2018–2020, Jupiter’s Great Red Spot interacted with series of anticyclones, losing part of its visible red area and distorting its shape The Great Red Spot (GRS) increased its tangential velocity; it did not change its vorticity, but did temporarily change its 90‐day oscillation in longitude Dynamical and radiative transfer modeling shows that the interactions affected the upper cloud of the GRS with no risk for its survival\n

\n\n\n

\n \n\n \n \n \n \n \n \n Automated Multi-Dataset Analysis (AMDA): An on-line database and analysis tool for heliospheric and planetary plasma data.\n \n \n \n \n\n\n \n Génot, V.; Budnik, E.; Jacquey, C.; Bouchemit, M.; Renard, B.; Dufourg, N.; André, N.; Cecconi, B.; Pitout, F.; Lavraud, B.; Fedorov, A.; Ganfloff, M.; Plotnikov, I.; Modolo, R.; Lormant, N.; Mohand, H. S. H.; Tao, C.; Besson, B.; Heulet, D.; Boucon, D.; Durand, J.; Bourrel, N.; Brzustowski, Q.; Jourdane, N.; Hitier, R.; Garnier, P.; Grison, B.; Aunai, N.; Jeandet, A.; and Cabrolie, F.\n\n\n \n\n\n\n Planetary and Space Science, 201: 105214. July 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Automated$ 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{genot_automated_2021,\n\ttitle = {Automated {Multi}-{Dataset} {Analysis} ({AMDA}): {An} on-line database and analysis tool for heliospheric and planetary plasma data},\n\tvolume = {201},\n\tissn = {0032-0633},\n\tshorttitle = {Automated {Multi}-{Dataset} {Analysis} ({AMDA})},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0032063321000532},\n\tdoi = {10.1016/j.pss.2021.105214},\n\tabstract = {Accessing, visualizing and analyzing heterogeneous plasma datasets has always been a tedious task that hindered students and senior researchers as well. Offering user friendly and versatile tools to perform basic research tasks is therefore pivotal for data centres including the Centre de Données de la Physique des Plasmas (CDPP http://www.cdpp.eu/) which holds a large variety of plasma data from various Earth, planetary and heliophysics missions and observatories in plasma physics. This clearly helps gaining increased attention, relevant feedback, and enhanced science return on data. These are the key ideas that crystallized at CDPP more than 15 years ago and resulted in the lay-out of the concepts, and then development, of AMDA, the Automated Multi-Dataset Analysis software (http://amda.cdpp.eu/). This paper gives a description of the architecture of AMDA, describes its functionalities, presents some use cases taken from the literature or fruitful collaborations and shows how it offers unique capabilities for educational purposes.},\n\tlanguage = {en},\n\turldate = {2023-06-28},\n\tjournal = {Planetary and Space Science},\n\tauthor = {Génot, V. and Budnik, E. and Jacquey, C. and Bouchemit, M. and Renard, B. and Dufourg, N. and André, N. and Cecconi, B. and Pitout, F. and Lavraud, B. and Fedorov, A. and Ganfloff, M. and Plotnikov, I. and Modolo, R. and Lormant, N. and Mohand, H. Si Hadj and Tao, C. and Besson, B. and Heulet, D. and Boucon, D. and Durand, J. and Bourrel, N. and Brzustowski, Q. and Jourdane, N. and Hitier, R. and Garnier, P. and Grison, B. and Aunai, N. and Jeandet, A. and Cabrolie, F.},\n\tmonth = jul,\n\tyear = {2021},\n\tkeywords = {Analysis tool, Database, Interoperability, Space plasmas},\n\tpages = {105214},\n}\n\n

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\n \n\n \n \n \n \n \n \n Dwarf planet (1) Ceres surface bluing due to high porosity resulting from sublimation.\n \n \n \n \n\n\n \n Schröder, S. E.; Poch, O.; Ferrari, M.; Angelis, S. D.; Sultana, R.; Potin, S. M.; Beck, P.; De Sanctis, M. C.; and Schmitt, B.\n\n\n \n\n\n\n Nature Communications, 12(1): 274. January 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Dwarf$ 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{schroder_dwarf_2021,\n\ttitle = {Dwarf planet (1) {Ceres} surface bluing due to high porosity resulting from sublimation},\n\tvolume = {12},\n\tissn = {2041-1723},\n\turl = {https://www.nature.com/articles/s41467-020-20494-5},\n\tdoi = {10.1038/s41467-020-20494-5},\n\tabstract = {Abstract \n            The Dawn mission found that the dominant colour variation on the surface of dwarf planet Ceres is a change of the visible spectral slope, where fresh impact craters are surrounded by blue (negative spectral-sloped) ejecta. The origin of this colour variation is still a mystery. Here we investigate a scenario in which an impact mixes the phyllosilicates present on the surface of Ceres with the water ice just below. In our experiment, Ceres analogue material is suspended in liquid water to create intimately mixed ice particles, which are sublimated under conditions approximating those on Ceres. The sublimation residue has a highly porous, foam-like structure made of phyllosilicates that scattered light in similar blue fashion as the Ceres surface. Our experiment provides a mechanism for the blue colour of fresh craters that can naturally emerge from the Ceres environment.},\n\tlanguage = {en},\n\tnumber = {1},\n\turldate = {2023-06-26},\n\tjournal = {Nature Communications},\n\tauthor = {Schröder, Stefan E. and Poch, Olivier and Ferrari, Marco and Angelis, Simone De and Sultana, Robin and Potin, Sandra M. and Beck, Pierre and De Sanctis, Maria Cristina and Schmitt, Bernard},\n\tmonth = jan,\n\tyear = {2021},\n\tpages = {274},\n}\n\n

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\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 = {2023-06-26},\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 Ice Chamber for Astrophysics–Astrochemistry (ICA): A new experimental facility for ion impact studies of astrophysical ice analogs.\n \n \n \n \n\n\n \n Herczku, P.; Mifsud, D. V.; Ioppolo, S.; Juhász, Z.; Kaňuchová, Z.; Kovács, S. T. S.; Traspas Muiña, A.; Hailey, P. A.; Rajta, I.; Vajda, I.; Mason, N. J.; McCullough, R. W.; Paripás, B.; and Sulik, B.\n\n\n \n\n\n\n Review of Scientific Instruments, 92(8): 084501. August 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 \n \n 1 download\n \n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@article{herczku_ice_2021,\n\ttitle = {The {Ice} {Chamber} for {Astrophysics}–{Astrochemistry} ({ICA}): {A} new experimental facility for ion impact studies of astrophysical ice analogs},\n\tvolume = {92},\n\tissn = {0034-6748, 1089-7623},\n\tshorttitle = {The {Ice} {Chamber} for {Astrophysics}–{Astrochemistry} ({ICA})},\n\turl = {https://pubs.aip.org/aip/rsi/article/1031744},\n\tdoi = {10.1063/5.0050930},\n\tlanguage = {en},\n\tnumber = {8},\n\turldate = {2023-06-26},\n\tjournal = {Review of Scientific Instruments},\n\tauthor = {Herczku, Péter and Mifsud, Duncan V. and Ioppolo, Sergio and Juhász, Zoltán and Kaňuchová, Zuzana and Kovács, Sándor T. S. and Traspas Muiña, Alejandra and Hailey, Perry A. and Rajta, István and Vajda, István and Mason, Nigel J. and McCullough, Robert W. and Paripás, Béla and Sulik, Béla},\n\tmonth = aug,\n\tyear = {2021},\n\tpages = {084501},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Microbial Survival and Adaptation in Extreme Terrestrial Environments—The Case of the Dallol Geothermal Area in Ethiopia.\n \n \n \n \n\n\n \n Cavalazzi, B.; and Sevasti, F.\n\n\n \n\n\n\n In Vukotić, B.; Gordon, R.; and Seckbach, J., editor(s), Planet Formation and Panspermia, pages 93–117. Wiley, 1 edition, October 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Microbial$ 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

@incollection{vukotic_microbial_2021,\n\tedition = {1},\n\ttitle = {Microbial {Survival} and {Adaptation} in {Extreme} {Terrestrial} {Environments}—{The} {Case} of the {Dallol} {Geothermal} {Area} in {Ethiopia}},\n\tisbn = {9781119640394 9781119640912},\n\turl = {https://onlinelibrary.wiley.com/doi/10.1002/9781119640912.ch6},\n\tlanguage = {en},\n\turldate = {2022-06-10},\n\tbooktitle = {Planet {Formation} and {Panspermia}},\n\tpublisher = {Wiley},\n\tauthor = {Cavalazzi, Barbara and Sevasti, Filippidou},\n\teditor = {Vukotić, Branislav and Gordon, Richard and Seckbach, Joseph},\n\tmonth = oct,\n\tyear = {2021},\n\tdoi = {10.1002/9781119640912.ch6},\n\tpages = {93--117},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n The Europlanet Evaluation Toolkit.\n \n \n \n \n\n\n \n Heward, A.; and DeWitt, J.\n\n\n \n\n\n\n In pages EPSC2021–275, September 2021. \n ADS Bibcode: 2021EPSC...15..275H\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{heward_europlanet_2021,\n\ttitle = {The {Europlanet} {Evaluation} {Toolkit}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2021EPSC...15..275H},\n\tdoi = {10.5194/epsc2021-275},\n\tabstract = {Evaluation can provide essential information in understanding the effectiveness and accessibility of outreach activities in engaging diverse communities. In this presentation, we will give an overview of the Europlanet Evaluation Toolkit, a resource that aims to empower outreach providers and educators in measuring and appraising the impact of their activities. The toolkit is intended to provide advice and resources that can be simply and easily integrated into normal outreach and education activities. It is available as an interactive online resource at http://www.europlanet-eu.org/europlanet-evaluation-toolkit/, as a downloadable PDF and as a hard copy (including a book and set of activity cards). The toolkit has been developed over a number of years with content provided by professional outreach evaluators Karen Bultitude and Jennifer DeWitt (UCL, UK). Initially, a series of focus groups and scoping discussions were held with active outreach providers from the planetary science community in order to determine what they wanted from such a toolkit, and what sort of tools would be of most interest. A shortlist of tools was developed based on these discussions, with volunteers testing out the tool instructions once they were drafted. The toolkit begins with a brief introduction to evaluation and steps to choosing the right tools. This advice takes the form of a series of questions to help design an evaluation approach and make the most efficient and effective use possible of limited time and resources. The toolkit offers a choice of 14 data collection tools that can be selected according to the audience (e.g. primary, secondary, interested adult, general public), the type of environment and activity (e.g. drop-in, interactive workshop, ongoing series, lecture/presentation or online) or according to when they might best be used (during, beginning/end, or after an event). The online version of the toolkit includes a set of interactive tables to help with the selection of which tool is most appropriate for any given situation. The toolkit includes descriptions and worked examples of how to use two techniques (word-clouds and thematic coding) to analyse the data, as well as some top tips for evaluation and recommended resources. For some of the tools, case study examples include information about how the tools have been used in the context of an event, how data was actually collected and analysed and what conclusions were reached, based on the data gathered. Over the past year, videos and training resources for using the toolkit have been added, as well as virtual alternatives to the physical tools. The Europlanet Evaluation Toolkit has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement No 871149 (Europlanet 2024 RI) and 654208 (Europlanet 2020 RI).},\n\turldate = {2023-02-25},\n\tauthor = {Heward, Anita and DeWitt, Jen},\n\tmonth = sep,\n\tyear = {2021},\n\tnote = {ADS Bibcode: 2021EPSC...15..275H},\n\tpages = {EPSC2021--275},\n}\n\n

\n\n\n

\n Evaluation can provide essential information in understanding the effectiveness and accessibility of outreach activities in engaging diverse communities. In this presentation, we will give an overview of the Europlanet Evaluation Toolkit, a resource that aims to empower outreach providers and educators in measuring and appraising the impact of their activities. The toolkit is intended to provide advice and resources that can be simply and easily integrated into normal outreach and education activities. It is available as an interactive online resource at http://www.europlanet-eu.org/europlanet-evaluation-toolkit/, as a downloadable PDF and as a hard copy (including a book and set of activity cards). The toolkit has been developed over a number of years with content provided by professional outreach evaluators Karen Bultitude and Jennifer DeWitt (UCL, UK). Initially, a series of focus groups and scoping discussions were held with active outreach providers from the planetary science community in order to determine what they wanted from such a toolkit, and what sort of tools would be of most interest. A shortlist of tools was developed based on these discussions, with volunteers testing out the tool instructions once they were drafted. The toolkit begins with a brief introduction to evaluation and steps to choosing the right tools. This advice takes the form of a series of questions to help design an evaluation approach and make the most efficient and effective use possible of limited time and resources. The toolkit offers a choice of 14 data collection tools that can be selected according to the audience (e.g. primary, secondary, interested adult, general public), the type of environment and activity (e.g. drop-in, interactive workshop, ongoing series, lecture/presentation or online) or according to when they might best be used (during, beginning/end, or after an event). The online version of the toolkit includes a set of interactive tables to help with the selection of which tool is most appropriate for any given situation. The toolkit includes descriptions and worked examples of how to use two techniques (word-clouds and thematic coding) to analyse the data, as well as some top tips for evaluation and recommended resources. For some of the tools, case study examples include information about how the tools have been used in the context of an event, how data was actually collected and analysed and what conclusions were reached, based on the data gathered. Over the past year, videos and training resources for using the toolkit have been added, as well as virtual alternatives to the physical tools. The Europlanet Evaluation Toolkit has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement No 871149 (Europlanet 2024 RI) and 654208 (Europlanet 2020 RI).\n

\n\n\n

\n \n\n \n \n \n \n \n \n Virtual european solar & planetary access (VESPA) 2021: consolidation.\n \n \n \n \n\n\n \n Erard, S.\n\n\n \n\n\n\n In European planetary science congress, pages EPSC2021–506, September 2021. \n tex.adsnote: Provided by the SAO/NASA Astrophysics Data System tex.adsurl: https://ui.adsabs.harvard.edu/abs/2021EPSC...15..506E tex.date-added: 2022-02-24 16:41:08 +0100 tex.date-modified: 2022-02-24 16:41:41 +0100 tex.eid: EPSC2021-506\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\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@inproceedings{2021EPSC...15..506E,\n\ttitle = {Virtual european solar \\& planetary access ({VESPA}) 2021: consolidation},\n\turl = {https://doi.org/10.5194/espc2021-506},\n\tdoi = {10.5194/espc2021-506},\n\tbooktitle = {European planetary science congress},\n\tauthor = {Erard, Stéphane},\n\tmonth = sep,\n\tyear = {2021},\n\tnote = {tex.adsnote: Provided by the SAO/NASA Astrophysics Data System\ntex.adsurl: https://ui.adsabs.harvard.edu/abs/2021EPSC...15..506E\ntex.date-added: 2022-02-24 16:41:08 +0100\ntex.date-modified: 2022-02-24 16:41:41 +0100\ntex.eid: EPSC2021-506},\n\tpages = {EPSC2021--506},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n Making the PDS planetary plasma interactions (PPI) node data accessible via the EPN-TAP protocol.\n \n \n \n\n\n \n Joy, S.; Moon, I. S.; Mafi, J.; Walker, R.; Cecconi, B.; and Erard, S.\n\n\n \n\n\n\n In AGU fall meeting abstracts, volume 2021, pages IN55F–0290, December 2021. \n tex.adsnote: Provided by the SAO/NASA Astrophysics Data System tex.adsurl: https://ui.adsabs.harvard.edu/abs/2021AGUFMIN55F0290J tex.eid: IN55F-0290\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{2021AGUFMIN55F0290J,\n\ttitle = {Making the {PDS} planetary plasma interactions ({PPI}) node data accessible via the {EPN}-{TAP} protocol},\n\tvolume = {2021},\n\tbooktitle = {{AGU} fall meeting abstracts},\n\tauthor = {Joy, Steven and Moon, In Sook and Mafi, Joseph and Walker, Raymond and Cecconi, Baptiste and Erard, Stephane},\n\tmonth = dec,\n\tyear = {2021},\n\tnote = {tex.adsnote: Provided by the SAO/NASA Astrophysics Data System\ntex.adsurl: https://ui.adsabs.harvard.edu/abs/2021AGUFMIN55F0290J\ntex.eid: IN55F-0290},\n\tpages = {IN55F--0290},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n New open source tools for MARSIS: providing access to SEG-Y data format for 3D analysis.\n \n \n \n \n\n\n \n Nodjoumi, G.; Guallini, L.; Orosei, R.; Penasa, L.; and Rossi, A. P.\n\n\n \n\n\n\n ,EGU21–4031. April 2021.\n ADS Bibcode: 2021EGUGA..23.4031N\n\n\n\n
\n\n\n\n \n \n $\"New$ 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{nodjoumi_new_2021,\n\ttitle = {New open source tools for {MARSIS}: providing access to {SEG}-{Y} data format for {3D} analysis.},\n\tshorttitle = {New open source tools for {MARSIS}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2021EGUGA..23.4031N},\n\tdoi = {10.5194/egusphere-egu21-4031},\n\tabstract = {The objective of this work is to present a new Free and Open-Source Software (FOSS) to read and convert to multiple data formats data acquired by the Mars Advanced Radar for Subsurface and Ionosphere Sounding (MARSIS) instrument on board Mars Express (MEX) orbiting Mars since 2005.MARSIS is an orbital synthetic aperture radar sounder that operates with dual-frequency between 1.3 and 5.5 MHz and wavelengths between 230 and 55 m for subsurface sounding. The Experiment Data Record (EDR) and Reduced Data Record (RDR) datasets are available for download on public access platforms such as the Planetary Science Archive fo ESA and the PDS-NASA Orbital Data Explorer (ODE).These datasets have been widely used for different research, focused to study the subsurface of the red planet up to a depth of a few kilometres, and especially for studying ice caps and looking for subsurface ice and water deposits, producing relevant results. (Lauro et al., 2020; Orosei et al., 2020)The Python tool presented here is capable of reading common data types used to distribute MARSIS dataset and then converting into multiple data formats. Users can interactively configure data source, destination, pre-processing and type of outputs among:Geopackages: for GIS software, is a single self-contained file containing a layer in which are stored all parameters for each file processed. Numpy array dump: for fast reading and analysis of original data for both frequencies. PNG images: for fast inspections, created for each frequency, and saved. Image pre-processing filters, such as image-denoising, standardization and normalization, can be selected by user. SEG-Y: for analysing data with seismic interpretation and processing software, see e.g. OpendTect, consist of a SEG-Y file for each frequency. SEG-Y capability is the most relevant feature, since is not present in any of other FOSS tool and give to researchers the possibility to visualize radargrams in advanced software, specific for seismic interpretation and analysis, making it possible to interpret the data in a fully three-dimensional environment.This tool, available on zenodo (Nodjoumi, 2021), has been developed completely in Python 3, relying only on open-source libraries, compatible with principal operating systems and with parallel processing capabilities, granting easy scalability and usability across a wide range of computing machines. It is also highly customizable since it can be expanded adding processing steps before export or new types of output. An additional module to ingest data directly into PostgreSQL/PostGIS and a module to interact directly with ACT-REACT interface of data platforms are under development.Acknowledgments:This study is within the Europlanet 2024 RI, and it has received funding from the European Union"s Horizon 2020 research and innovation programme under grant agreement No 871149. References:Lauro, S. E. et al. (2020) "Multiple subglacial water bodies below the south pole of Mars unveiled by new MARSIS data", doi: 10.1038/s41550-020-1200-6.Nodjoumi, G. (2021) 'MARSIS-xDR-READER', doi: 10.5281/zenodo.4436199Orosei, R. et al. (2020) "The global search for liquid water on mars from orbit: Current and future perspectives", doi: 10.3390/life10080120.},\n\turldate = {2023-02-25},\n\tauthor = {Nodjoumi, Giacomo and Guallini, Luca and Orosei, Roberto and Penasa, Luca and Rossi, Angelo Pio},\n\tmonth = apr,\n\tyear = {2021},\n\tnote = {ADS Bibcode: 2021EGUGA..23.4031N},\n\tpages = {EGU21--4031},\n}\n\n

\n\n\n

\n The objective of this work is to present a new Free and Open-Source Software (FOSS) to read and convert to multiple data formats data acquired by the Mars Advanced Radar for Subsurface and Ionosphere Sounding (MARSIS) instrument on board Mars Express (MEX) orbiting Mars since 2005.MARSIS is an orbital synthetic aperture radar sounder that operates with dual-frequency between 1.3 and 5.5 MHz and wavelengths between 230 and 55 m for subsurface sounding. The Experiment Data Record (EDR) and Reduced Data Record (RDR) datasets are available for download on public access platforms such as the Planetary Science Archive fo ESA and the PDS-NASA Orbital Data Explorer (ODE).These datasets have been widely used for different research, focused to study the subsurface of the red planet up to a depth of a few kilometres, and especially for studying ice caps and looking for subsurface ice and water deposits, producing relevant results. (Lauro et al., 2020; Orosei et al., 2020)The Python tool presented here is capable of reading common data types used to distribute MARSIS dataset and then converting into multiple data formats. Users can interactively configure data source, destination, pre-processing and type of outputs among:Geopackages: for GIS software, is a single self-contained file containing a layer in which are stored all parameters for each file processed. Numpy array dump: for fast reading and analysis of original data for both frequencies. PNG images: for fast inspections, created for each frequency, and saved. Image pre-processing filters, such as image-denoising, standardization and normalization, can be selected by user. SEG-Y: for analysing data with seismic interpretation and processing software, see e.g. OpendTect, consist of a SEG-Y file for each frequency. SEG-Y capability is the most relevant feature, since is not present in any of other FOSS tool and give to researchers the possibility to visualize radargrams in advanced software, specific for seismic interpretation and analysis, making it possible to interpret the data in a fully three-dimensional environment.This tool, available on zenodo (Nodjoumi, 2021), has been developed completely in Python 3, relying only on open-source libraries, compatible with principal operating systems and with parallel processing capabilities, granting easy scalability and usability across a wide range of computing machines. It is also highly customizable since it can be expanded adding processing steps before export or new types of output. An additional module to ingest data directly into PostgreSQL/PostGIS and a module to interact directly with ACT-REACT interface of data platforms are under development.Acknowledgments:This study is within the Europlanet 2024 RI, and it has received funding from the European Union\"s Horizon 2020 research and innovation programme under grant agreement No 871149. References:Lauro, S. E. et al. (2020) \"Multiple subglacial water bodies below the south pole of Mars unveiled by new MARSIS data\", doi: 10.1038/s41550-020-1200-6.Nodjoumi, G. (2021) 'MARSIS-xDR-READER', doi: 10.5281/zenodo.4436199Orosei, R. et al. (2020) \"The global search for liquid water on mars from orbit: Current and future perspectives\", doi: 10.3390/life10080120.\n

\n\n\n

\n \n\n \n \n \n \n \n \n Mercury's exospheric model for SPIDER.\n \n \n \n \n\n\n \n Moroni, M.; Mura, A.; Milillo, A.; and Nicolas, A.\n\n\n \n\n\n\n ,EGU21–7583. April 2021.\n ADS Bibcode: 2021EGUGA..23.7583M\n\n\n\n
\n\n\n\n \n \n $\"Mercury's$ 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{moroni_mercurys_2021,\n\ttitle = {Mercury's exospheric model for {SPIDER}},\n\turl = {https://ui.adsabs.harvard.edu/abs/2021EGUGA..23.7583M},\n\tdoi = {10.5194/egusphere-egu21-7583},\n\tabstract = {The propagation of Solar events and the response of planetary environment is a fundamental area of interest in the study of the solar system, object of several models and tools for data analysis. In the framework of the starting Europlanet-2024 program, the Virtual Activity (VA) SPIDER (Sun-Planet Interactions Digital Environment on Request) aims a publicly available and sophisticated services, in order to model planetary environments and solar wind interactions. One of these services is focused on the prototype for the model of the Mercury exosphere, in particular to study its exospheric density and the solar wind precipitation to the surface. Mercury is a unique case in the solar system: absence of an atmosphere and the weakness of the intrinsic magnetic field. The Hermean exosphere is continuously eroded and refilled by interactions with plasma and surface, so the environment is considered as a single, unified system - surface- exosphere-magnetosphere. The study of the generation mechanisms, the compositions and the configuration of the Hermean exosphere will provide crucial insight in the planet status and evolution. The MESSENGER/NASA mission visited Mercury in the period 2008-2015, adding a consistent amount of data but a global description of planet"s exosphere is still not available; the ESA BepiColombo mission will study Mercury orbiting around the planet from 2025. For this reason, it is important to have a modelling tool ready for interpreting observational data and testing different hypothesis on release mechanism. Considering different generation and loss mechanisms, we present a Monte Carlo three-dimensional model of the Hermean exosphere, that considers all the major sources and loss mechanisms. In fact, this numerical model includes among the processes responsible of the formation of such an exosphere the ion sputtering (IS), the thermal desorption (TD), the photon-stimulated desorption (PSD) and micro-meteoroids impact vaporization (MMIV) from the planetary surface. The model calculates the trajectories of ejected particles from which we obtain the spatial and energy distributions of atmospheric particles. Furthermore, an analytical model is obtained by fitting the numerical data with parametric functions. In this way, it is possible to model the exosphere of Mercury for each source separately and we can investigate the role of each physical source independently of the others. Here we present the web-based interface of the model and the functionalities of this infrastructure that is being implemented in SPIDER. This project has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement No 871149.},\n\turldate = {2023-02-25},\n\tauthor = {Moroni, Martina and Mura, Alessandro and Milillo, Anna and Nicolas, Andrè},\n\tmonth = apr,\n\tyear = {2021},\n\tnote = {ADS Bibcode: 2021EGUGA..23.7583M},\n\tpages = {EGU21--7583},\n}\n\n

\n\n\n

\n The propagation of Solar events and the response of planetary environment is a fundamental area of interest in the study of the solar system, object of several models and tools for data analysis. In the framework of the starting Europlanet-2024 program, the Virtual Activity (VA) SPIDER (Sun-Planet Interactions Digital Environment on Request) aims a publicly available and sophisticated services, in order to model planetary environments and solar wind interactions. One of these services is focused on the prototype for the model of the Mercury exosphere, in particular to study its exospheric density and the solar wind precipitation to the surface. Mercury is a unique case in the solar system: absence of an atmosphere and the weakness of the intrinsic magnetic field. The Hermean exosphere is continuously eroded and refilled by interactions with plasma and surface, so the environment is considered as a single, unified system - surface- exosphere-magnetosphere. The study of the generation mechanisms, the compositions and the configuration of the Hermean exosphere will provide crucial insight in the planet status and evolution. The MESSENGER/NASA mission visited Mercury in the period 2008-2015, adding a consistent amount of data but a global description of planet\"s exosphere is still not available; the ESA BepiColombo mission will study Mercury orbiting around the planet from 2025. For this reason, it is important to have a modelling tool ready for interpreting observational data and testing different hypothesis on release mechanism. Considering different generation and loss mechanisms, we present a Monte Carlo three-dimensional model of the Hermean exosphere, that considers all the major sources and loss mechanisms. In fact, this numerical model includes among the processes responsible of the formation of such an exosphere the ion sputtering (IS), the thermal desorption (TD), the photon-stimulated desorption (PSD) and micro-meteoroids impact vaporization (MMIV) from the planetary surface. The model calculates the trajectories of ejected particles from which we obtain the spatial and energy distributions of atmospheric particles. Furthermore, an analytical model is obtained by fitting the numerical data with parametric functions. In this way, it is possible to model the exosphere of Mercury for each source separately and we can investigate the role of each physical source independently of the others. Here we present the web-based interface of the model and the functionalities of this infrastructure that is being implemented in SPIDER. This project has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement No 871149.\n

\n\n\n

\n \n\n \n \n \n \n \n \n Amateur astronomy support to current and future space missions: From the 2010s to the 2030s.\n \n \n \n \n\n\n \n Hueso, R.; Fletcher, L.; Orton, G.; Sánchez-Lavega, A.; Hansen, C.; Rogers, J.; Mousis, O.; Delcroix, M.; and Scherf, M.\n\n\n \n\n\n\n Technical Report EPSC2021-80, Copernicus Meetings, June 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Amateur$ 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

@techreport{hueso_amateur_2021,\n\ttitle = {Amateur astronomy support to current and future space missions: {From} the 2010s to the 2030s},\n\tshorttitle = {Amateur astronomy support to current and future space missions},\n\turl = {https://meetingorganizer.copernicus.org/EPSC2021/EPSC2021-80.html},\n\tlanguage = {en},\n\tnumber = {EPSC2021-80},\n\turldate = {2023-02-25},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Hueso, Ricardo and Fletcher, Leigh and Orton, Glenn and Sánchez-Lavega, Agustín and Hansen, Candice and Rogers, John and Mousis, Olivier and Delcroix, Marc and Scherf, Manuel},\n\tmonth = jun,\n\tyear = {2021},\n\tdoi = {10.5194/epsc2021-80},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Spectral variability of brigth regions whitin Kuiper quadrangle: spectral indication for integrated geostratigraphic maps.\n \n \n \n \n\n\n \n Carli, C.; Giacomini, L.; Zambon, F.; Galluzzi, V.; Ferrari, S.; Massironi, M.; Altieri, F.; Ferranti, L.; Palumbo, P.; and Capaccioni, F.\n\n\n \n\n\n\n Technical Report EPSC2021-238, Copernicus Meetings, June 2021.\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\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@techreport{carli_spectral_2021,\n\ttitle = {Spectral variability of brigth regions whitin {Kuiper} quadrangle: spectral indication for integrated geostratigraphic maps},\n\tshorttitle = {Spectral variability of brigth regions whitin {Kuiper} quadrangle},\n\turl = {https://meetingorganizer.copernicus.org/EPSC2021/EPSC2021-238.html},\n\tlanguage = {en},\n\tnumber = {EPSC2021-238},\n\turldate = {2023-02-25},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Carli, Cristian and Giacomini, Lorenza and Zambon, Francesca and Galluzzi, Valentina and Ferrari, Sabrina and Massironi, Matteo and Altieri, Francesca and Ferranti, Luigi and Palumbo, Pasquale and Capaccioni, Fabrizio},\n\tmonth = jun,\n\tyear = {2021},\n\tdoi = {10.5194/epsc2021-238},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Virtual Workshop on the use of the Europlanet Telescope Networkfor amateur astronomers: An experience from the Spanish-Portuguese hub of the Europlanet Society.\n \n \n \n \n\n\n \n Garate-Lopez, I.; Álvaro, J.; Hueso, R.; Gilli, G.; Ordóñez-Etxeberria, I.; Nogues, R. N.; Correa, M.; Campàs, M.; and Scherf, M.\n\n\n \n\n\n\n Technical Report EPSC2021-304, Copernicus Meetings, June 2021.\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\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@techreport{garate-lopez_virtual_2021,\n\ttitle = {Virtual {Workshop} on the use of the {Europlanet} {Telescope} {Networkfor} amateur astronomers: {An} experience from the {Spanish}-{Portuguese} hub of the {Europlanet} {Society}},\n\tshorttitle = {Virtual {Workshop} on the use of the {Europlanet} {Telescope} {Networkfor} amateur astronomers},\n\turl = {https://meetingorganizer.copernicus.org/EPSC2021/EPSC2021-304.html},\n\tlanguage = {en},\n\tnumber = {EPSC2021-304},\n\turldate = {2023-02-25},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Garate-Lopez, Itziar and Álvaro, Joaquín and Hueso, Ricardo and Gilli, Gabriella and Ordóñez-Etxeberria, Iñaki and Nogues, Ramón Navès and Correa, Mercè and Campàs, Montse and Scherf, Manuel},\n\tmonth = jun,\n\tyear = {2021},\n\tdoi = {10.5194/epsc2021-304},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n GMAP – European Mapping efforts for Geologic Mapping of Planetary bodies.\n \n \n \n \n\n\n \n Nass, A.; Massironi, M.; Rossi, A. P.; Penasa, L.; Pozzobon, R.; Brandt, C.; Nodjoumi, G.; Pondrelli, M.; Pantaloni, M.; Galluzzi, V.; Altieri, F.; Frigeri, A.; Carli, C.; Giacomini, L.; Mège, D.; Gurgurewicz, J.; Tesson, P.; Marinangeli, L.; Bogert, C. v. d.; and Poehler, C.\n\n\n \n\n\n\n Technical Report EPSC2021-383, Copernicus Meetings, June 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"GMAP$ 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

@techreport{nass_gmap_2021,\n\ttitle = {{GMAP} \\&ndash; {European} {Mapping} efforts for {Geologic} {Mapping} of {Planetary} bodies},\n\turl = {https://meetingorganizer.copernicus.org/EPSC2021/EPSC2021-383.html},\n\tlanguage = {en},\n\tnumber = {EPSC2021-383},\n\turldate = {2023-02-25},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Nass, Andrea and Massironi, Matteo and Rossi, Angelo Pio and Penasa, Luca and Pozzobon, Riccardo and Brandt, Carlos and Nodjoumi, Giacomo and Pondrelli, Monica and Pantaloni, Marco and Galluzzi, Vallentina and Altieri, Francesca and Frigeri, Alessandro and Carli, Christian and Giacomini, Lorenza and Mège, Daniel and Gurgurewicz, Joanna and Tesson, Pierre-Antoine and Marinangeli, Lucia and Bogert, Carolyn van der and Poehler, Claudia},\n\tmonth = jun,\n\tyear = {2021},\n\tdoi = {10.5194/epsc2021-383},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Supporting the planetary sciences community with the Europlanet Telescope Network.\n \n \n \n \n\n\n \n Scherf, M.; Snodgrass, C.; Tautvaisiene, G.; Hueso, R.; Podlewska-Gaca, E.; Colas, F.; Garate-Lopez, I.; Langner, K.; and Kargl, G.\n\n\n \n\n\n\n Technical Report EPSC2021-549, Copernicus Meetings, June 2021.\n \n\n\n\n
\n\n\n\n \n \n $\"Supporting$ 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 1 download\n \n \n\n \n \n \n \n \n \n \n\n \n \n \n\n\n\n

@techreport{scherf_supporting_2021,\n\ttitle = {Supporting the planetary sciences community with the {Europlanet} {Telescope} {Network}},\n\turl = {https://meetingorganizer.copernicus.org/EPSC2021/EPSC2021-549.html},\n\tlanguage = {en},\n\tnumber = {EPSC2021-549},\n\turldate = {2023-02-25},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Scherf, Manuel and Snodgrass, Colin and Tautvaisiene, Grazina and Hueso, Ricardo and Podlewska-Gaca, Edyta and Colas, Francois and Garate-Lopez, Itziar and Langner, Krzysztof and Kargl, Günter},\n\tmonth = jun,\n\tyear = {2021},\n\tdoi = {10.5194/epsc2021-549},\n}\n\n

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

\n\n

\n \n 2020\n \n \n (15)\n \n \n

\n \n \n

\n \n\n \n \n \n \n \n \n Kuiper Quadrangle spectral analysis: looking forward to integrated geological map.\n \n \n \n \n\n\n \n Carli, C.; Giacomini, L.; Zambon, F.; Ferrari, S.; Massironi, M.; Galluzzi, V.; Altieri, F.; Capaccioni, F.; Ferranti, L.; and Palumbo, P.\n\n\n \n\n\n\n In pages EPSC2020–367, 2020. \n \n\n\n\n
\n\n\n\n \n \n $\"Kuiper$ 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

@inproceedings{carli_kuiper_2020,\n\ttitle = {Kuiper {Quadrangle} spectral analysis: looking forward to integrated geological map},\n\turl = {https://www.europlanet-society.org/wp-content/uploads/2024/02/375.pdf},\n\tauthor = {Carli, Cristian and Giacomini, Lorenza and Zambon, Francesca and Ferrari, Sabrina and Massironi, Matteo and Galluzzi, Valentina and Altieri, Francesca and Capaccioni, Fabrizio and Ferranti, Luigi and Palumbo, Pasquale},\n\tyear = {2020},\n\tpages = {EPSC2020--367},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Automatic detection of magnetopause and bow shock crossing signatures in MESSENGER magnetometer data.\n \n \n \n \n\n\n \n Lavrukhin, A.; Parunakian, D.; Nevskiy, D.; Amerstorfer, U.; Windisch, A.; Julka, S.; Möstl, C.; Reiss, M.; and Bailey, R.\n\n\n \n\n\n\n Technical Report EPSC2020-826, Copernicus Meeting, September 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Automatic$ 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

@techreport{lavrukhin_automatic_2020,\n\ttype = {conference presentation},\n\ttitle = {Automatic detection of magnetopause and bow shock crossing signatures in {MESSENGER} magnetometer data},\n\turl = {https://www.europlanet-society.org/wp-content/uploads/2024/02/253-1.pdf},\n\tabstract = {The magnetosphere of Mercury is rather small and highly dynamic, due to its weak internal magnetic field and its close proximity to the Sun. The changing solar wind conditions principally determine the locations of both the Hermean bow shock and magnetopause. In 2011 – 2015 MESSENGER spacecraft completed more than 4000 orbits around Mercury, thus giving a data of more than 8000 crossings of bow shock and magnetopause of the planet. This makes it possible to study in detail the bow shock, the magnetopause and the magnetosheath structures.\n\nIn this work, we determine crossings of the bow shock and the magnetopause of Mercury by applying machine learning methods to the MESSENGER magnetometer data. We try to identify the crossings for the complete orbital mission and model the average three-dimensional shape of these boundaries depending on the external interplanetary magnetic field (IMF). Further, we try to clarify the dependence of the two boundary locations on the heliocentric distance of Mercury and on the solar activity cycle phase. Also, we study the effect of the IMF partial penetration into the Hermean magnetosphere. The results are compared with the obtained previously in other works.\n\nThis work may be of interest for future Mercury research related to the BepiColombo spacecraft mission, which will enter the orbit around the planet at December 2025.},\n\tlanguage = {English},\n\tnumber = {EPSC2020-826},\n\tinstitution = {Copernicus Meeting},\n\tauthor = {Lavrukhin, A. and Parunakian, D. and Nevskiy, D. and Amerstorfer, U. and Windisch, A. and Julka, S. and Möstl, C. and Reiss, M. and Bailey, R.},\n\tmonth = sep,\n\tyear = {2020},\n}\n\n

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

\n\n\n

\n \n\n \n \n \n \n \n \n Spatial and Open Research Data Infrastructure for Planetary Science - Lessons learned from European developments.\n \n \n \n \n\n\n \n Nass, A.; Asch, K.; Gasselt, S. v.; and Rossi, A. P.\n\n\n \n\n\n\n Technical Report EPSC2020-1058, Copernicus Meetings, August 2020.\n Conference Name: EPSC2020\n\n\n\n
\n\n\n\n \n \n $\"Spatial$ 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

@techreport{nass_spatial_2020,\n\ttitle = {Spatial and {Open} {Research} {Data} {Infrastructure} for {Planetary} {Science} - {Lessons} learned from {European} developments},\n\turl = {https://www.europlanet-society.org/wp-content/uploads/2024/02/192.pdf},\n\tlanguage = {en},\n\tnumber = {EPSC2020-1058},\n\turldate = {2021-03-14},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Nass, Andrea and Asch, Kristine and Gasselt, Stephan van and Rossi, Angelo Pio},\n\tmonth = aug,\n\tyear = {2020},\n\tdoi = {10.5194/epsc2020-1058},\n\tnote = {Conference Name: EPSC2020},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Reflectance spectroscopy of ammonium-bearing minerals: a tool to improve the knowledge of the icy planetary bodies.\n \n \n \n \n\n\n \n Fastelli, M.; Comodi, P.; Piergallini, R.; Maturilli, A.; Balic-Zunic, T.; and Zucchini, A.\n\n\n \n\n\n\n ,EPSC2020–294. September 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Reflectance$ 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{fastelli_reflectance_2020,\n\ttitle = {Reflectance spectroscopy of ammonium-bearing minerals: a tool to improve the knowledge of the icy planetary bodies},\n\tshorttitle = {Reflectance spectroscopy of ammonium-bearing minerals},\n\turl = {https://www.europlanet-society.org/wp-content/uploads/2024/02/191.pdf},\n\tabstract = {Recent discoveries demonstrated that the surface of Mars, Ceres and other celestial bodies like asteroids and comets are characterized by the presence of ammonium bearing minerals (Dalle Ore et al., 2018; Berg et al., 2016, Poch et al., 2020). Data collected by New Horizon LORRI and Ralph emphasized the presence of ammonia on Charon, one of the Pluto"s satellites, that is, ammonium chloride, ammonium nitrate and ammonium carbonate have been claimed as the best candidates for its composition (Cook et al., 2018). Moreover, the analysis of the absorption features of Mars spectra at {\\textasciitilde}1.07, 1.31 and 1.57 μm can be related to ammonium bearing minerals (Sefton-Nash et al., 2012) as well as the presence of oceans underneath the Europa"s crust (Zimmer et al., 2000) suggests a hypothetical composition of water + ammonia, as anti-freezing water element (Sphon and Schubert, 2003). In this scenario, cryovolcanism activity (Jia et al., 2018) can give rise to an interaction between water ammonia and the surface.This study focuses on, by taking into account sulfates, phosphates, aluminates and borates, understanding how different anionic groups and the different amount of water, affect the ammonium spectra features. Ammonium bearing minerals are of significant interest as hydrogen bonds can affect the NH4+ absorption features and the configuration of the hydrogen bonds, N-H….X, in ammonium salts (e.g. NH4Cl, NH4Br), can be quite different (Harlov et al., 2001).All this, with a careful analysis of remote data compared with the analyses of more accurate laboratory data, should allow a better remote characterization of planetary bodies.In this work, the reflectance spectra of some ammoniated hydrous and anhydrous salts, namely sal-ammoniac NH4Cl, larderellite NH4B5O7(OH)2·H2O, mascagnite (NH4)SO4, struvite (NH4)MgPO4·6H2O and tschermigite (NH4)Al(SO4)2·12H2O, were collected at room temperature and at 193K. These samples were selected to improve the NH4-bearing mineral reflectance spectra database and to extend the investigated spectral range with respect to the literature data: e.g. Berg et al., 2016.We analyzed natural ammonium bearing minerals using reflectance spectroscopy in the long-wave ultraviolet (UV), visible, near-infrared (NIR), and mid-infrared (MIR) regions ({\\textasciitilde}1 - 16 μm) at 298 and 198 K. In addition, thermogravimetric analysis (TG) and differential scanning calorimetry (DSC) were made to evaluate the amount of water/ammonium loss and the potential phase transitions occurring in the investigated temperature range. X-ray diffraction analyses were performed on the samples before and after thermal treatments to study the evolution of their crystal structure.Reflectance spectra of ammoniated minerals show absorption features at 1.3, 1.6, 2.06, 2.14, 3, 3.23, 5.8 and 7.27 μm, related to ammonium group. The 2ν3 at {\\textasciitilde}1.56 μm and the ν3+ν4 at {\\textasciitilde}2.13 μm, are the most affected modes by crystal structure type, since their position is strictly related to hydrogen bonds. The reflectance spectra of water-rich samples (struvite (NH4)MgPO4·6(H2O) and tschermigite (NH4)Al(SO4)2·12(H2O)) show only fundamental absorption features in the area from 2 to 2.8 μm and a strong water feature at 3 μm. An endothermic peak at 192° C was detected in the DSC diagram of sal-ammoniac sample, due to the phase transition from CsCl structure type to NaCl type.Important was the application of a new proprietary tool (areal mixing model RE-Mix) created to fit remote sensing data coming from planetary bodies with a mixing of the reflectance spectra of single minerals. The RE-Mix tool is based on Hapke model, the most common scattering theory used to calculate synthetic reflectance spectra (Hapke, 1981, 2012). We can assume that the surfaces of planetary bodies contain mixtures of different minerals. In the interpretation of the remote sensing data, it is therefore necessary to assume a mixture of spectra of different minerals. The spectral modelling method used inside Re-Mix is an areal mixing model, which is the most used and the least computationally intensive process. It is based on the least-squares method and the goodness of fit (χ2) is adjusted changing the weight coefficients of the single minerals. The tool is based on Wolfram Mathematica software (Wolfram 1999). A full graphical interface was developed.The method interprets the remote sensing data from Jupiter"s moon, Europa and Ceres asteroid. We found a number of NH4-bearing mineral mixtures can fit the planetary spectra together with other mineral species, improving the hypothesis that ammonium species should be among the non-icy materials present on the surface of Galilean moons and mixed with carbonate mineral on Ceres surface.These knowledges will give us more detailed information from the remote data and suggestions which areas and data should have higher priority for remote investigations in the future space missions.References:Berg, Breanne L., et al. "Reflectance spectroscopy (0.35-8 μm) of ammonium-bearing minerals and qualitative comparison to Ceres-like asteroids." Icarus 265 (2016): 218-237. Cook, Jason C., et al. "Composition of Pluto"s small satellites: Analysis of New Horizons spectral images." Icarus 315 (2018): 30-45. Dalle Ore, C. Morea, et al. "Ices on Charon: Distribution of H2O and NH3 from New Horizons LEISA observations." Icarus 300 (2018): 21-32. Hapke, B. (1981). Bidirectional reflectance spectroscopy: 1. Theory. Journal of Geophysical Research: Solid Earth, 86(B4), 3039-3054. Hapke, B. (2012). Theory of reflectance and emittance spectroscopy. Cambridge university press. Harlov, D. E., M. Andrut, and B. Pöter. "Characterisation of tobelite (NH4)Al2 [AlSi3O10](OH2) and ND4-tobelite (ND4)Al2 [AlSi3O10](OD)2 using IR spectroscopy and Rietveld refinement of XRD spectra." Physics and Chemistry of Minerals 28.4 (2001): 268-276. Jia, Xianzhe, et al. "Evidence of a plume on Europa from Galileo magnetic and plasma wave signatures." Nature Astronomy 2.6 (2018): 459-464. Poch, Olivier, et al. "Ammonium salts are a reservoir of nitrogen on a cometary nucleus and possibly on some asteroids." Science 367.6483 (2020). Sefton-Nash, E., et al. "Topographic, spectral and thermal inertia analysis of interior layered deposits in Iani Chaos, Mars." Icarus 221.1 (2012): 20-42. Spohn, Tilman, and Gerald Schubert. "Oceans in the icy Galilean satellites of Jupiter?." Icarus 161.2 (2003): 456-467. Wolfram, Stephen. The MATHEMATICA® book, version 4. Cambridge university press, 1999. Zimmer, Christophe, Krishan K. Khurana, and Margaret G. Kivelson. "Subsurface oceans on Europa and Callisto: Constraints from Galileo magnetometer observations." Icarus 147.2 (2000): 329-347.},\n\turldate = {2021-07-25},\n\tauthor = {Fastelli, Maximiliano and Comodi, Paola and Piergallini, Riccardo and Maturilli, Alessandro and Balic-Zunic, Tonci and Zucchini, Azzurra},\n\tmonth = sep,\n\tyear = {2020},\n\tpages = {EPSC2020--294},\n}\n\n

\n\n\n

\n Recent discoveries demonstrated that the surface of Mars, Ceres and other celestial bodies like asteroids and comets are characterized by the presence of ammonium bearing minerals (Dalle Ore et al., 2018; Berg et al., 2016, Poch et al., 2020). Data collected by New Horizon LORRI and Ralph emphasized the presence of ammonia on Charon, one of the Pluto\"s satellites, that is, ammonium chloride, ammonium nitrate and ammonium carbonate have been claimed as the best candidates for its composition (Cook et al., 2018). Moreover, the analysis of the absorption features of Mars spectra at ~1.07, 1.31 and 1.57 μm can be related to ammonium bearing minerals (Sefton-Nash et al., 2012) as well as the presence of oceans underneath the Europa\"s crust (Zimmer et al., 2000) suggests a hypothetical composition of water + ammonia, as anti-freezing water element (Sphon and Schubert, 2003). In this scenario, cryovolcanism activity (Jia et al., 2018) can give rise to an interaction between water ammonia and the surface.This study focuses on, by taking into account sulfates, phosphates, aluminates and borates, understanding how different anionic groups and the different amount of water, affect the ammonium spectra features. Ammonium bearing minerals are of significant interest as hydrogen bonds can affect the NH4+ absorption features and the configuration of the hydrogen bonds, N-H….X, in ammonium salts (e.g. NH4Cl, NH4Br), can be quite different (Harlov et al., 2001).All this, with a careful analysis of remote data compared with the analyses of more accurate laboratory data, should allow a better remote characterization of planetary bodies.In this work, the reflectance spectra of some ammoniated hydrous and anhydrous salts, namely sal-ammoniac NH4Cl, larderellite NH4B5O7(OH)2·H2O, mascagnite (NH4)SO4, struvite (NH4)MgPO4·6H2O and tschermigite (NH4)Al(SO4)2·12H2O, were collected at room temperature and at 193K. These samples were selected to improve the NH4-bearing mineral reflectance spectra database and to extend the investigated spectral range with respect to the literature data: e.g. Berg et al., 2016.We analyzed natural ammonium bearing minerals using reflectance spectroscopy in the long-wave ultraviolet (UV), visible, near-infrared (NIR), and mid-infrared (MIR) regions (~1 - 16 μm) at 298 and 198 K. In addition, thermogravimetric analysis (TG) and differential scanning calorimetry (DSC) were made to evaluate the amount of water/ammonium loss and the potential phase transitions occurring in the investigated temperature range. X-ray diffraction analyses were performed on the samples before and after thermal treatments to study the evolution of their crystal structure.Reflectance spectra of ammoniated minerals show absorption features at 1.3, 1.6, 2.06, 2.14, 3, 3.23, 5.8 and 7.27 μm, related to ammonium group. The 2ν3 at ~1.56 μm and the ν3+ν4 at ~2.13 μm, are the most affected modes by crystal structure type, since their position is strictly related to hydrogen bonds. The reflectance spectra of water-rich samples (struvite (NH4)MgPO4·6(H2O) and tschermigite (NH4)Al(SO4)2·12(H2O)) show only fundamental absorption features in the area from 2 to 2.8 μm and a strong water feature at 3 μm. An endothermic peak at 192° C was detected in the DSC diagram of sal-ammoniac sample, due to the phase transition from CsCl structure type to NaCl type.Important was the application of a new proprietary tool (areal mixing model RE-Mix) created to fit remote sensing data coming from planetary bodies with a mixing of the reflectance spectra of single minerals. The RE-Mix tool is based on Hapke model, the most common scattering theory used to calculate synthetic reflectance spectra (Hapke, 1981, 2012). We can assume that the surfaces of planetary bodies contain mixtures of different minerals. In the interpretation of the remote sensing data, it is therefore necessary to assume a mixture of spectra of different minerals. The spectral modelling method used inside Re-Mix is an areal mixing model, which is the most used and the least computationally intensive process. It is based on the least-squares method and the goodness of fit (χ2) is adjusted changing the weight coefficients of the single minerals. The tool is based on Wolfram Mathematica software (Wolfram 1999). A full graphical interface was developed.The method interprets the remote sensing data from Jupiter\"s moon, Europa and Ceres asteroid. We found a number of NH4-bearing mineral mixtures can fit the planetary spectra together with other mineral species, improving the hypothesis that ammonium species should be among the non-icy materials present on the surface of Galilean moons and mixed with carbonate mineral on Ceres surface.These knowledges will give us more detailed information from the remote data and suggestions which areas and data should have higher priority for remote investigations in the future space missions.References:Berg, Breanne L., et al. \"Reflectance spectroscopy (0.35-8 μm) of ammonium-bearing minerals and qualitative comparison to Ceres-like asteroids.\" Icarus 265 (2016): 218-237. Cook, Jason C., et al. \"Composition of Pluto\"s small satellites: Analysis of New Horizons spectral images.\" Icarus 315 (2018): 30-45. Dalle Ore, C. Morea, et al. \"Ices on Charon: Distribution of H2O and NH3 from New Horizons LEISA observations.\" Icarus 300 (2018): 21-32. Hapke, B. (1981). Bidirectional reflectance spectroscopy: 1. Theory. Journal of Geophysical Research: Solid Earth, 86(B4), 3039-3054. Hapke, B. (2012). Theory of reflectance and emittance spectroscopy. Cambridge university press. Harlov, D. E., M. Andrut, and B. Pöter. \"Characterisation of tobelite (NH4)Al2 [AlSi3O10](OH2) and ND4-tobelite (ND4)Al2 [AlSi3O10](OD)2 using IR spectroscopy and Rietveld refinement of XRD spectra.\" Physics and Chemistry of Minerals 28.4 (2001): 268-276. Jia, Xianzhe, et al. \"Evidence of a plume on Europa from Galileo magnetic and plasma wave signatures.\" Nature Astronomy 2.6 (2018): 459-464. Poch, Olivier, et al. \"Ammonium salts are a reservoir of nitrogen on a cometary nucleus and possibly on some asteroids.\" Science 367.6483 (2020). Sefton-Nash, E., et al. \"Topographic, spectral and thermal inertia analysis of interior layered deposits in Iani Chaos, Mars.\" Icarus 221.1 (2012): 20-42. Spohn, Tilman, and Gerald Schubert. \"Oceans in the icy Galilean satellites of Jupiter?.\" Icarus 161.2 (2003): 456-467. Wolfram, Stephen. The MATHEMATICA® book, version 4. Cambridge university press, 1999. Zimmer, Christophe, Krishan K. Khurana, and Margaret G. Kivelson. \"Subsurface oceans on Europa and Callisto: Constraints from Galileo magnetometer observations.\" Icarus 147.2 (2000): 329-347.\n

\n\n\n

\n \n\n \n \n \n \n \n \n SSHADE, its solid spectra databases and its future band list of molecular solids.\n \n \n \n \n\n\n \n Schmitt, B.; Bollard, P.; Albert, D.; Bonal, L.; and Poch, O.\n\n\n \n\n\n\n Technical Report EPSC2020-644, Copernicus Meetings, August 2020.\n Conference Name: EPSC2020\n\n\n\n
\n\n\n\n \n \n $\"SSHADE,$ 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

@techreport{schmitt_sshade_2020,\n\ttitle = {{SSHADE}, its solid spectra databases and its future band list of molecular solids},\n\turl = {https://www.europlanet-society.org/wp-content/uploads/2024/02/190.pdf},\n\tlanguage = {en},\n\tnumber = {EPSC2020-644},\n\turldate = {2021-02-20},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Schmitt, Bernard and Bollard, Philippe and Albert, Damien and Bonal, Lydie and Poch, Olivier},\n\tmonth = aug,\n\tyear = {2020},\n\tdoi = {https://doi.org/10.5194/epsc2020-644},\n\tdoi = {https://doi.org/10.5194/epsc2020-644},\n\tnote = {Conference Name: EPSC2020},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Constructing and deconstructing geological maps: a QGIS plugin for creating topologically consistent geological cartography.\n \n \n \n \n\n\n \n Penasa, L.; Frigeri, A.; Pozzobon, R.; Brandt, C. H; De Toffoli, B.; Naß, A.; Rossi, A. P.; and Massironi, M.\n\n\n \n\n\n\n In European planetary science congress, pages EPSC2020–1057, 2020. \n \n\n\n\n
\n\n\n\n \n \n $\"Constructing$ 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

@inproceedings{penasa2020constructing,\n\ttitle = {Constructing and deconstructing geological maps: a {QGIS} plugin for creating topologically consistent geological cartography},\n\turl = {https://www.europlanet-society.org/wp-content/uploads/2024/02/179.pdf},\n\tbooktitle = {European planetary science congress},\n\tauthor = {Penasa, Luca and Frigeri, Alessandro and Pozzobon, Riccardo and Brandt, Carlos H and De Toffoli, Barbara and Naß, Andrea and Rossi, Angelo Pio and Massironi, Matteo},\n\tyear = {2020},\n\tpages = {EPSC2020--1057},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Geological and geomorphological mapping of Martian sedimentary deposits: an attempt to identify current practices in mapping and representation.\n \n \n \n \n\n\n \n Pondrelli, M.; Frigeri, A.; Marinangeli, L.; Di Pietro, I.; Pantaloni, M.; Pozzobon, R.; Nass, A.; and Rossi, A. P.\n\n\n \n\n\n\n ,EPSC2020–232. September 2020.\n Conference Name: European Planetary Science Congress ADS Bibcode: 2020EPSC...14..232P\n\n\n\n
\n\n\n\n \n \n $\"Geological$ 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{2020EPSC...14..232P,\n\ttitle = {Geological and geomorphological mapping of {Martian} sedimentary deposits: an attempt to identify current practices in mapping and representation},\n\tshorttitle = {Geological and geomorphological mapping of {Martian} sedimentary deposits},\n\turl = {https://www.europlanet-society.org/wp-content/uploads/2023/12/CO-Meeting-Organizer-EPSC2020-232.pdf},\n\tabstract = {The quantity, quality, and type of available datasets on Mars have improved in the last couple of decades. Context Camera (CTX) (Malin et al., 2007) on board the NASA Mars Reconnaissance Orbiter (MRO) provides a global coverage with an average resolution of 6 meters/pixel while the High Resolution Imaging Science Experiment (HiRISE) on board MRO (McEwen et al., 2007) allows up to 30 cm/pixel analyses at the local scale. These data allow at places also the DTM generation, but extensive topographic reconstructions at an average scale of 50 meters/pixel are possible using the High Resolution Stereo Camera (HRSC) on board of ESA Mars Express (MEX) (Neukum et al., 2004). Moreover compositional constraints can be provided by the spectral data coming from Observatoire pour la Minéralogie, l"Eau, les Glaces, et l"Activité (OMEGA) on board MEX and from Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) on board the NASA Mars Reconnaissance Orbiter (MRO) (Murchie et al., 2007). These relatively recent datasets coupled with the older datasets and Geographical Information Systems (GIS) provide an impressive suite of tools to develop meaningful planetary geological maps. In principle, these new data allow to add to the traditional geomorphological or chronostratigraphic mapping approaches, also a geological map approach somewhat akin to the one well-known on Earth, although, a "true" geological map should be based on the lithological characters of the mapped units; using tone, texture, absence/presence of sedimentary structure, and, if possible, compositional hints to define the units, may represent an adequate "planetary perspective", obviously in addition to the stratigraphic position within the succession. This map approach has the advantages to be relatively objective (and so potentially more useful for geological context analyses) and to represent the stratigraphic complexity within a region. This approach is complementary to the more interpretative (because it includes the processes/environments of formation of the different features) one of the geomorphological maps, which has the obvious advantage to describe the environments/processes active in the region. In the framework of the GMAP (Geologic MApping of Planetary bodies) project, we present here an attempt to merge these two cartographic products taking advantage of GIS-based tools. Moreover, we aim at testing, where possible, the Earth-born symbols designed for the Geological Map of Italy (ISPRA, 2009, 2018) to try to make the "language" of geological maps as uniform as possible. In order to perform these analyses, we selected a series of putative fluvio-lacustrine landforms located in Holden crater, along the south-eastern inner rim (coordinates 26.9°S-33.5°W). The geological map allowed to distinguish several units separated by unconformities. In particular, the Impact unit, equivalent to the one recognized by Tanaka et al. (2014) is nonconformably covered by the materials located inside the crater and along the crater rim. These materials can be distinguished in two groups separated by a disconformity, the first characterized by a relatively large lateral extension of the units and the second by a scattered appearance of the units. Within the first group, a disconformity separates a lower part from the upper part of the succession. The geomorphological map allows to genetically interpret these units, defining: i) a first impact stage, correspondent to the emplacement of Holden crater, ii) a "water-related" phase (correspondent to the lower group of the geological map), and iii) an aeolian phase made of mega-ripples and dunes (correspondent to the upper group of the geological map). The "water-related" phase can be further divided in a fluvio-lacustrine and a glacial phase.We propose the realization of a unique geologic and geomorphologic product that includes a polygon layer with the geological units map described above, a linear layer with the unit contacts (i.e., stratigraphic characterization), and a linear shapefile with tectonic features and geomorphological interpretations. The polygonal units" layer might be also suitable to subdivide the units in lower-order ranked units, using appropriate fields (i.e., formation/members on Earth). This approach might be best suited for projects developed at the local scale, similar to what is done on Earth, while a chronostratigraphic approach is more fitting and recommended at the regional and global scale. We will identify a possible set of graphical symbols describing the surface features, locating potential limits in current GIS symbology implementation.The GMAP project represents an opportunity to share our experience and to collect current practices in planetary and terrestrial geological and geomorphological mapping, identifying what elements are still lacking and need to be discussed or developed. GMAP and Europlanet 2024 RI have received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement\nNo 871149. ReferencesISPRA (2009) - Carta Geologica d"Italia. Guida alla rappresentazione cartografica. Modifiche e integrazioni ai Quaderni 2/1996 e 6/1997. Roma, pp. 166ISPRA (2018) - Carta Geomorfologica d"Italia. Guida alla rappresentazione cartografica. Modifiche e integrazioni al Quaderno 4/1994. Roma, pp. 95Malin, M. C., J. F. Bell, B. A. Cantor, M. A. Caplinger, W. M. Calvin, T. R. Clancy, K. S. Edgett, L. Edwards, R. M. Haberle, and P. B. James (2007), Context camera investigation on board the Mars Reconnaissance Orbiter, Journal of Geophysical Research: Planets(1991-2012), 112(E5).McEwen, A. S., E. M. Eliason, J. W. Bergstrom, N. T. Bridges, C. J. Hansen, A. W. Delamere, J. A. Grant, V. C. Gulick, K. E. Herkenhoff, and L. Keszthelyi (2007), Mars reconnaissance orbiter"s high resolution imaging science experiment (HiRISE), Journal of Geophysical Research: Planets (1991-2012), 112(E5).Murchie, S. et al. (2009), Evidence for the origin of layered deposits in Candor Chasma, Mars, from mineral composition and hydrologic modeling, Journal of Geophysical Research: Planets, 114, E00D05, doi:10.1029/2009je003343.Neukum, G, R Jaumann, and H. the and Team (2004), HRSC—The High Resolution Stereo Camera of Mars Express, European Space Agency Special Publication, SP-1240, 17-35.Tanaka, K., J. Skinner, J. Dohm, R. Irwin, E. Kolb, C. Fortezzo, T. Platz, G. Michael, and T. Hare (2014), Geologic map of Mars, USGS Scientific Investigations Map 3292, doi:10.3133/sim3292.},\n\turldate = {2021-09-02},\n\tauthor = {Pondrelli, Monica and Frigeri, Alessandro and Marinangeli, Lucia and Di Pietro, Ilaria and Pantaloni, Marco and Pozzobon, Riccardo and Nass, Andrea and Rossi, Angelo Pio},\n\tmonth = sep,\n\tyear = {2020},\n\tnote = {Conference Name: European Planetary Science Congress\nADS Bibcode: 2020EPSC...14..232P},\n\tpages = {EPSC2020--232},\n}\n\n

\n\n\n

\n The quantity, quality, and type of available datasets on Mars have improved in the last couple of decades. Context Camera (CTX) (Malin et al., 2007) on board the NASA Mars Reconnaissance Orbiter (MRO) provides a global coverage with an average resolution of 6 meters/pixel while the High Resolution Imaging Science Experiment (HiRISE) on board MRO (McEwen et al., 2007) allows up to 30 cm/pixel analyses at the local scale. These data allow at places also the DTM generation, but extensive topographic reconstructions at an average scale of 50 meters/pixel are possible using the High Resolution Stereo Camera (HRSC) on board of ESA Mars Express (MEX) (Neukum et al., 2004). Moreover compositional constraints can be provided by the spectral data coming from Observatoire pour la Minéralogie, l\"Eau, les Glaces, et l\"Activité (OMEGA) on board MEX and from Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) on board the NASA Mars Reconnaissance Orbiter (MRO) (Murchie et al., 2007). These relatively recent datasets coupled with the older datasets and Geographical Information Systems (GIS) provide an impressive suite of tools to develop meaningful planetary geological maps. In principle, these new data allow to add to the traditional geomorphological or chronostratigraphic mapping approaches, also a geological map approach somewhat akin to the one well-known on Earth, although, a \"true\" geological map should be based on the lithological characters of the mapped units; using tone, texture, absence/presence of sedimentary structure, and, if possible, compositional hints to define the units, may represent an adequate \"planetary perspective\", obviously in addition to the stratigraphic position within the succession. This map approach has the advantages to be relatively objective (and so potentially more useful for geological context analyses) and to represent the stratigraphic complexity within a region. This approach is complementary to the more interpretative (because it includes the processes/environments of formation of the different features) one of the geomorphological maps, which has the obvious advantage to describe the environments/processes active in the region. In the framework of the GMAP (Geologic MApping of Planetary bodies) project, we present here an attempt to merge these two cartographic products taking advantage of GIS-based tools. Moreover, we aim at testing, where possible, the Earth-born symbols designed for the Geological Map of Italy (ISPRA, 2009, 2018) to try to make the \"language\" of geological maps as uniform as possible. In order to perform these analyses, we selected a series of putative fluvio-lacustrine landforms located in Holden crater, along the south-eastern inner rim (coordinates 26.9°S-33.5°W). The geological map allowed to distinguish several units separated by unconformities. In particular, the Impact unit, equivalent to the one recognized by Tanaka et al. (2014) is nonconformably covered by the materials located inside the crater and along the crater rim. These materials can be distinguished in two groups separated by a disconformity, the first characterized by a relatively large lateral extension of the units and the second by a scattered appearance of the units. Within the first group, a disconformity separates a lower part from the upper part of the succession. The geomorphological map allows to genetically interpret these units, defining: i) a first impact stage, correspondent to the emplacement of Holden crater, ii) a \"water-related\" phase (correspondent to the lower group of the geological map), and iii) an aeolian phase made of mega-ripples and dunes (correspondent to the upper group of the geological map). The \"water-related\" phase can be further divided in a fluvio-lacustrine and a glacial phase.We propose the realization of a unique geologic and geomorphologic product that includes a polygon layer with the geological units map described above, a linear layer with the unit contacts (i.e., stratigraphic characterization), and a linear shapefile with tectonic features and geomorphological interpretations. The polygonal units\" layer might be also suitable to subdivide the units in lower-order ranked units, using appropriate fields (i.e., formation/members on Earth). This approach might be best suited for projects developed at the local scale, similar to what is done on Earth, while a chronostratigraphic approach is more fitting and recommended at the regional and global scale. We will identify a possible set of graphical symbols describing the surface features, locating potential limits in current GIS symbology implementation.The GMAP project represents an opportunity to share our experience and to collect current practices in planetary and terrestrial geological and geomorphological mapping, identifying what elements are still lacking and need to be discussed or developed. GMAP and Europlanet 2024 RI have received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement No 871149. ReferencesISPRA (2009) - Carta Geologica d\"Italia. Guida alla rappresentazione cartografica. Modifiche e integrazioni ai Quaderni 2/1996 e 6/1997. Roma, pp. 166ISPRA (2018) - Carta Geomorfologica d\"Italia. Guida alla rappresentazione cartografica. Modifiche e integrazioni al Quaderno 4/1994. Roma, pp. 95Malin, M. C., J. F. Bell, B. A. Cantor, M. A. Caplinger, W. M. Calvin, T. R. Clancy, K. S. Edgett, L. Edwards, R. M. Haberle, and P. B. James (2007), Context camera investigation on board the Mars Reconnaissance Orbiter, Journal of Geophysical Research: Planets(1991-2012), 112(E5).McEwen, A. S., E. M. Eliason, J. W. Bergstrom, N. T. Bridges, C. J. Hansen, A. W. Delamere, J. A. Grant, V. C. Gulick, K. E. Herkenhoff, and L. Keszthelyi (2007), Mars reconnaissance orbiter\"s high resolution imaging science experiment (HiRISE), Journal of Geophysical Research: Planets (1991-2012), 112(E5).Murchie, S. et al. (2009), Evidence for the origin of layered deposits in Candor Chasma, Mars, from mineral composition and hydrologic modeling, Journal of Geophysical Research: Planets, 114, E00D05, doi:10.1029/2009je003343.Neukum, G, R Jaumann, and H. the and Team (2004), HRSC—The High Resolution Stereo Camera of Mars Express, European Space Agency Special Publication, SP-1240, 17-35.Tanaka, K., J. Skinner, J. Dohm, R. Irwin, E. Kolb, C. Fortezzo, T. Platz, G. Michael, and T. Hare (2014), Geologic map of Mars, USGS Scientific Investigations Map 3292, doi:10.3133/sim3292.\n

\n\n\n

\n \n\n \n \n \n \n \n \n PLANMAP data packaging: lessons learned towards FAIR planetary geologic maps.\n \n \n \n \n\n\n \n Brandt, C. H.; Rossi, A. P.; Penasa, L.; Pozzobon, R.; Luzzi, E.; Wright, J.; Carli, C.; and Massironi, M.\n\n\n \n\n\n\n Technical Report pico, March 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"PLANMAP$ 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

@techreport{brandt_planmap_2020,\n\ttype = {other},\n\ttitle = {{PLANMAP} data packaging: lessons learned towards {FAIR} planetary geologic maps},\n\tshorttitle = {{PLANMAP} data packaging},\n\turl = {https://meetingorganizer.copernicus.org/EGU2020/EGU2020-18839.html},\n\tabstract = {\\&lt;p\\&gt;Geologic mapping is a key element of planetary exploration for mission planning, orbital and rover reconnaissance, and target selection for in-situ analysis and sample return, as well as for understanding the formation and evolution of planetary surfaces. The PLANMAP project (http://www.planmap.eu) aims at produce high-level, standardized geological maps of the Moon, Mars, and Mercury (Massironi M. et al., 2018). The project is integrating different types of data as images, spectral-cubes, chemical data, Digital Terrain Models and three-dimensional geological models to produce geological maps suitable to planetary exploration at different levels. The process results in rich datasets composed by a variety of datatypes encapsulated in open standards and released to the community as freely accessible packages (https://maps.planmap.eu).\\&lt;br\\&gt;To accomplish the complexity of deploying PLANMAP packages, considering reliability and automation as key components of a data release workflow, we arranged a data management framework respecting the FAIR (findable, accessible, interoperable, and reusable) guidelines. Geographic data are stored and served by a multi-layered Web-GIS allowing easy information discovery. Particular attention has been paid in designing the user interface and in the definition of the underlying data structure. Different data query services are also provided to properly address different user needs (Luzzi E. et al., 2020). PLANMAP\\&amp;\\#8217;s datasets can be downloaded in the form of fully contained packages (https://data.planmap.eu) fulfilling a specifically designed standard. Once a data package is ready for publication, validation and summary information extraction take place and the results are published together within the packages.\\&lt;br\\&gt;We will here present an overview of the PLANMAP\\&amp;\\#8217;s deployed data system, and the technical solutions that were adopted with the final goal of improving the quality standards of planetary geological maps.\\&lt;/p\\&gt;\\&lt;p\\&gt;References:\\&lt;/p\\&gt;\\&lt;p\\&gt;- Luzzi E. et al., 2020, \\&amp;\\#8220;Tectono-magmatic, Sedimentary and Hydrothermal History of Arsinoes and Pyrrhae Chaos, Mars.\\&amp;\\#8221;, EarthArXiv, doi:10.31223/osf.io/td297\\&lt;/p\\&gt;\\&lt;p\\&gt;- Massironi M. et al., 2018, \\&amp;\\#8220;Towards integrated geological maps and 3D geo-models of planetary surfaces: the H2020 PLANetary MAPping project\\&amp;\\#8221;, EGU General Assembly 2018\\&lt;/p\\&gt;},\n\turldate = {2023-06-29},\n\tinstitution = {pico},\n\tauthor = {Brandt, Carlos Henrique and Rossi, Angelo Pio and Penasa, Luca and Pozzobon, Riccardo and Luzzi, Erica and Wright, Jack and Carli, Cristian and Massironi, Matteo},\n\tmonth = mar,\n\tyear = {2020},\n\tdoi = {10.5194/egusphere-egu2020-18839},\n}\n\n

\n\n\n

\n Geologic mapping is a key element of planetary exploration for mission planning, orbital and rover reconnaissance, and target selection for in-situ analysis and sample return, as well as for understanding the formation and evolution of planetary surfaces. The PLANMAP project (http://www.planmap.eu) aims at produce high-level, standardized geological maps of the Moon, Mars, and Mercury (Massironi M. et al., 2018). The project is integrating different types of data as images, spectral-cubes, chemical data, Digital Terrain Models and three-dimensional geological models to produce geological maps suitable to planetary exploration at different levels. The process results in rich datasets composed by a variety of datatypes encapsulated in open standards and released to the community as freely accessible packages (https://maps.planmap.eu). To accomplish the complexity of deploying PLANMAP packages, considering reliability and automation as key components of a data release workflow, we arranged a data management framework respecting the FAIR (findable, accessible, interoperable, and reusable) guidelines. Geographic data are stored and served by a multi-layered Web-GIS allowing easy information discovery. Particular attention has been paid in designing the user interface and in the definition of the underlying data structure. Different data query services are also provided to properly address different user needs (Luzzi E. et al., 2020). PLANMAP’s datasets can be downloaded in the form of fully contained packages (https://data.planmap.eu) fulfilling a specifically designed standard. Once a data package is ready for publication, validation and summary information extraction take place and the results are published together within the packages. We will here present an overview of the PLANMAP’s deployed data system, and the technical solutions that were adopted with the final goal of improving the quality standards of planetary geological maps.References:- Luzzi E. et al., 2020, “Tectono-magmatic, Sedimentary and Hydrothermal History of Arsinoes and Pyrrhae Chaos, Mars.”, EarthArXiv, doi:10.31223/osf.io/td297- Massironi M. et al., 2018, “Towards integrated geological maps and 3D geo-models of planetary surfaces: the H2020 PLANetary MAPping project”, EGU General Assembly 2018\n

\n\n\n

\n \n\n \n \n \n \n \n \n Image Processing Utils.\n \n \n \n \n\n\n \n Nodjoumi, G.\n\n\n \n\n\n\n October 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Image$ 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

@misc{nodjoumi_image_2020,\n\ttitle = {Image {Processing} {Utils}},\n\tcopyright = {GNU General Public License v2.0 or later, Open Access},\n\turl = {https://zenodo.org/record/4153464},\n\tabstract = {No description provided.},\n\turldate = {2023-06-29},\n\tpublisher = {Zenodo},\n\tauthor = {Nodjoumi, Giacomo},\n\tmonth = oct,\n\tyear = {2020},\n\tdoi = {10.5281/ZENODO.4153464},\n}\n\n

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\n\n\n

\n \n\n \n \n \n \n \n \n Identifying Flux Rope Signatures Using a Deep Neural Network.\n \n \n \n \n\n\n \n Dos Santos, L. F. G.; Narock, A.; Nieves-Chinchilla, T.; Nuñez, M.; and Kirk, M.\n\n\n \n\n\n\n Solar Physics, 295(10): 131. October 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Identifying$ 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{dos_santos_identifying_2020,\n\ttitle = {Identifying {Flux} {Rope} {Signatures} {Using} a {Deep} {Neural} {Network}},\n\tvolume = {295},\n\tissn = {0038-0938, 1573-093X},\n\turl = {https://link.springer.com/10.1007/s11207-020-01697-x},\n\tdoi = {10.1007/s11207-020-01697-x},\n\tlanguage = {en},\n\tnumber = {10},\n\turldate = {2023-06-29},\n\tjournal = {Solar Physics},\n\tauthor = {Dos Santos, Luiz F. G. and Narock, Ayris and Nieves-Chinchilla, Teresa and Nuñez, Marlon and Kirk, Michael},\n\tmonth = oct,\n\tyear = {2020},\n\tpages = {131},\n}\n\n

\n\n\n\n

\n\n\n

\n \n\n \n \n \n \n \n \n Danakil Depression: a multi-sensorial experience.\n \n \n \n \n\n\n \n Cavalazzi, B.; Tistoni, S.; Altobelli, F.; and Heward, A.\n\n\n \n\n\n\n In August 2020. Copernicus Meetings\n \n\n\n\n
\n\n\n\n \n \n $\"Danakil$ 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

@inproceedings{cavalazzi_danakil_2020,\n\ttitle = {Danakil {Depression}: a multi-sensorial experience},\n\tshorttitle = {Danakil {Depression}},\n\turl = {https://meetingorganizer.copernicus.org/EPSC2020/EPSC2020-1050.html},\n\tlanguage = {en},\n\turldate = {2023-02-25},\n\tpublisher = {Copernicus Meetings},\n\tauthor = {Cavalazzi, Barbara and Tistoni, Samantha and Altobelli, Francesco and Heward, Anita},\n\tmonth = aug,\n\tyear = {2020},\n\tdoi = {10.5194/epsc2020-1050},\n}\n\n

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\n \n\n \n \n \n \n \n \n The Europlanet Telescope Network: A global collaboration in support of planetary sciences.\n \n \n \n \n\n\n \n Scherf, M.; Snodgrass, C.; Hueso, R.; Tautvaisiene, G.; Podlewska-Gaca, E.; Colas, F.; Sanchez-Lavega, A.; Garate-Lopez, I.; Dudziński, G.; Bartczak, P.; and Kargl, G.\n\n\n \n\n\n\n Technical Report EPSC2020-313, Copernicus Meetings, August 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

@techreport{scherf_europlanet_2020,\n\ttitle = {The {Europlanet} {Telescope} {Network}: {A} global collaboration in support of planetary sciences},\n\tshorttitle = {The {Europlanet} {Telescope} {Network}},\n\turl = {https://meetingorganizer.copernicus.org/EPSC2020/EPSC2020-313.html},\n\tlanguage = {en},\n\tnumber = {EPSC2020-313},\n\turldate = {2023-02-25},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Scherf, Manuel and Snodgrass, Colin and Hueso, Ricardo and Tautvaisiene, Grazina and Podlewska-Gaca, Edyta and Colas, Francois and Sanchez-Lavega, Agustín and Garate-Lopez, Itziar and Dudziński, Grzegorz and Bartczak, Przemyslaw and Kargl, Günter},\n\tmonth = aug,\n\tyear = {2020},\n\tdoi = {10.5194/epsc2020-313},\n}\n\n

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\n \n\n \n \n \n \n \n \n Planets in a Room: an educational tool for Europlanet.\n \n \n \n \n\n\n \n Giacomini, L.; Aloisi, F.; Angelis, I. D.; and Capretti, S.\n\n\n \n\n\n\n Technical Report EPSC2020-916, Copernicus Meetings, August 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Planets$ 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

@techreport{giacomini_planets_2020,\n\ttitle = {Planets in a {Room}: an educational tool for {Europlanet}},\n\tshorttitle = {Planets in a {Room}},\n\turl = {https://meetingorganizer.copernicus.org/EPSC2020/EPSC2020-916.html},\n\tlanguage = {en},\n\tnumber = {EPSC2020-916},\n\turldate = {2023-02-25},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Giacomini, Livia and Aloisi, Francesco and Angelis, Ilaria De and Capretti, Stefano},\n\tmonth = aug,\n\tyear = {2020},\n\tdoi = {10.5194/epsc2020-916},\n}\n\n

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\n \n\n \n \n \n \n \n \n Ion and electron impact studies on astrophysically relevant ices: a new laboratory at Atomki in Debrecen.\n \n \n \n \n\n\n \n Herczku, P.; Juhász, Z.; Kovács, S. T. S.; Sulik, B.; Ioppolo, S.; Mason, N. J.; Mifsud, D. V.; Traspas-Muina, A.; Czentye, M.; Kanuchová, Z.; Paripás, B.; and McCullough, R. W.\n\n\n \n\n\n\n Technical Report EPSC2020-950, Copernicus Meetings, August 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Ion$ 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

@techreport{herczku_ion_2020,\n\ttitle = {Ion and electron impact studies on astrophysically relevant ices: a new laboratory at {Atomki} in {Debrecen}},\n\tshorttitle = {Ion and electron impact studies on astrophysically relevant ices},\n\turl = {https://meetingorganizer.copernicus.org/EPSC2020/EPSC2020-950.html},\n\tlanguage = {en},\n\tnumber = {EPSC2020-950},\n\turldate = {2023-02-25},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Herczku, Péter and Juhász, Zoltán and Kovács, Sándor T. S. and Sulik, Béla and Ioppolo, Sergio and Mason, Nigel J. and Mifsud, Duncan V. and Traspas-Muina, Alejandra and Czentye, Máté and Kanuchová, Zuzana and Paripás, Béla and McCullough, Robert W.},\n\tmonth = aug,\n\tyear = {2020},\n\tdoi = {10.5194/epsc2020-950},\n}\n\n

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\n \n\n \n \n \n \n \n \n Amateur Ground-based Support of the first BepiColombo flyby of Venus.\n \n \n \n \n\n\n \n Garate-Lopez, I.; Hueso, R.; Lee, Y. J.; Mangano, V.; Jessup, K. L.; Peralta, J.; Sanchez-Lavega, A.; Zender, J.; Benkhoff, J.; Murakami, G.; and Scherf, M.\n\n\n \n\n\n\n Technical Report EPSC2020-1060, Copernicus Meetings, August 2020.\n \n\n\n\n
\n\n\n\n \n \n $\"Amateur$ 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

@techreport{garate-lopez_amateur_2020,\n\ttitle = {Amateur {Ground}-based {Support} of the first {BepiColombo} flyby of {Venus}},\n\turl = {https://meetingorganizer.copernicus.org/EPSC2020/EPSC2020-1060.html},\n\tlanguage = {en},\n\tnumber = {EPSC2020-1060},\n\turldate = {2023-02-25},\n\tinstitution = {Copernicus Meetings},\n\tauthor = {Garate-Lopez, Itziar and Hueso, Ricardo and Lee, Yeon Joo and Mangano, Valeria and Jessup, Kandis Lea and Peralta, Javier and Sanchez-Lavega, Agustin and Zender, Joe and Benkhoff, Johannes and Murakami, Go and Scherf, Manuel},\n\tmonth = aug,\n\tyear = {2020},\n\tdoi = {10.5194/epsc2020-1060},\n}\n\n

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\n \n undefined\n \n \n (1)\n \n \n

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\n \n\n \n \n \n \n \n \n Software Infrastructure on the publishing of planetary geo-morphological maps.\n \n \n \n \n\n\n \n Brandt, C. H; Penasa, L.; and Rossi, A. P\n\n\n \n\n\n\n . .\n \n\n\n\n
\n\n\n\n \n \n $\"Software$ 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{brandt_software_nodate,\n\ttitle = {Software {Infrastructure} on the publishing of planetary geo-morphological maps},\n\turl = {https://www.researchgate.net/publication/364210041_Software_Infrastructure_on_the_publishing_of_planetary_geo-morphological_maps},\n\tauthor = {Brandt, Carlos H and Penasa, Luca and Rossi, Angelo P},\n}\n\n

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