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\n  \n 2023\n \n \n (1)\n \n \n
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\n \n\n \n \n \n \n \n \n Aeolian dust resuspension on Mars studied using a recirculating environmental wind tunnel.\n \n \n \n \n\n\n \n Waza, A.; Kjer, J.; Peiteado, M.; Jardiel, T.; Iversen, J.; Rasmussen, K.; and Merrison, J.\n\n\n \n\n\n\n Planetary and Space Science, 227: 105638. March 2023.\n \n\n\n\n
\n\n\n\n \n \n \"AeolianPaper\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 1 download\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
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@article{waza_aeolian_2023,\n\ttitle = {Aeolian dust resuspension on {Mars} studied using a recirculating environmental wind tunnel},\n\tvolume = {227},\n\tissn = {0032-0633},\n\turl = {https://www.sciencedirect.com/science/article/pii/S0032063323000077},\n\tdoi = {10.1016/j.pss.2023.105638},\n\tabstract = {In this laboratory investigation, Mars dust analogues have been mobilized by wind flow under Martian conditions of low density CO2. Various laser based techniques have been employed to quantify dust mobilization and suspension; these include 2D laser Doppler velocimetry, optical opacity and optical reflectance. Direct mobilization of dust has been observed with a threshold shear stress as low as around 0.036 ​± ​0.007 ​Pa though only for dust layers of {\\textgreater}1 monolayer and at a flux as high as 220 ​± ​100 ​mg/m2/s at around 20\\% above threshold. The dust resuspension fluxes for this direct process have been measured to be significantly lower (order of magnitude) than the mobilization rate, typically around 10 ​mg/m2/s at a shear stress of 0.15 ​Pa. This mechanism involved the removal, transport and breakup of dust aggregates. In another mechanism, saltating sand was seen to remobilize deposited dust layers {\\textless}1 monolayer at a similar mobilization flux of around 50 ​± ​20 ​mg/m2/s and with a threshold of around 0.08 ​± ​0.008 ​Pa. At the high wind speeds used in these studies a significant fraction of the saltating sand grains become transported at relatively high elevation ({\\textgreater}10 ​cm) and to high velocity. These essentially suspended grains were seen to generate a large flux of dust through impact abrasion. This constitutes a potential mechanism for dust generation on Mars, though is beyond the scope of this study to isolate and investigate.},\n\tlanguage = {en},\n\turldate = {2023-02-25},\n\tjournal = {Planetary and Space Science},\n\tauthor = {Waza, A. and Kjer, J. and Peiteado, M. and Jardiel, T. and Iversen, J. and Rasmussen, K. and Merrison, J.},\n\tmonth = mar,\n\tyear = {2023},\n\tkeywords = {Aeolian, Dust, Mars, Sand},\n\tpages = {105638},\n}\n
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\n In this laboratory investigation, Mars dust analogues have been mobilized by wind flow under Martian conditions of low density CO2. Various laser based techniques have been employed to quantify dust mobilization and suspension; these include 2D laser Doppler velocimetry, optical opacity and optical reflectance. Direct mobilization of dust has been observed with a threshold shear stress as low as around 0.036 ​± ​0.007 ​Pa though only for dust layers of \\textgreater1 monolayer and at a flux as high as 220 ​± ​100 ​mg/m2/s at around 20% above threshold. The dust resuspension fluxes for this direct process have been measured to be significantly lower (order of magnitude) than the mobilization rate, typically around 10 ​mg/m2/s at a shear stress of 0.15 ​Pa. This mechanism involved the removal, transport and breakup of dust aggregates. In another mechanism, saltating sand was seen to remobilize deposited dust layers \\textless1 monolayer at a similar mobilization flux of around 50 ​± ​20 ​mg/m2/s and with a threshold of around 0.08 ​± ​0.008 ​Pa. At the high wind speeds used in these studies a significant fraction of the saltating sand grains become transported at relatively high elevation (\\textgreater10 ​cm) and to high velocity. These essentially suspended grains were seen to generate a large flux of dust through impact abrasion. This constitutes a potential mechanism for dust generation on Mars, though is beyond the scope of this study to isolate and investigate.\n
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\n  \n 2022\n \n \n (1)\n \n \n
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\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
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@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
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