Insights into Martian bedform migration: Results from Gale, Jezero and Pasteur craters
Anurag Sahu
Department of Earth and Atmospheric Sciences, National Institute of Technology Rourkela, Odisha, India
Search for more papers by this authorAnirban Mandal
Department of Earth and Atmospheric Sciences, National Institute of Technology Rourkela, Odisha, India
Search for more papers by this authorSatyaki Banerjee
Department of Earth and Atmospheric Sciences, National Institute of Technology Rourkela, Odisha, India
Search for more papers by this authorCorresponding Author
Jagabandhu Panda
Department of Earth and Atmospheric Sciences, National Institute of Technology Rourkela, Odisha, India
Correspondence
Jagabandhu Panda, Department of Earth and Atmospheric Sciences, National Institute of Technology Rourkela, Odisha 769008, India.
Email: [email protected]
Search for more papers by this authorAnurag Sahu
Department of Earth and Atmospheric Sciences, National Institute of Technology Rourkela, Odisha, India
Search for more papers by this authorAnirban Mandal
Department of Earth and Atmospheric Sciences, National Institute of Technology Rourkela, Odisha, India
Search for more papers by this authorSatyaki Banerjee
Department of Earth and Atmospheric Sciences, National Institute of Technology Rourkela, Odisha, India
Search for more papers by this authorCorresponding Author
Jagabandhu Panda
Department of Earth and Atmospheric Sciences, National Institute of Technology Rourkela, Odisha, India
Correspondence
Jagabandhu Panda, Department of Earth and Atmospheric Sciences, National Institute of Technology Rourkela, Odisha 769008, India.
Email: [email protected]
Search for more papers by this authorAbstract
An attempt is made in this study to advance the understanding of the sand movement on Mars by studying the bedform migration at Gale, Jezero and Pasteur craters. The study on the grain size distribution at Gale Crater using Curiosity rover (MAHLI and APXS) observations reveals that the grains with smaller diameters (~50–150 μ) are more prone to migration and vice-versa, which gives an idea of the necessary requirements that initiate bedform migration. The chemical analysis of the surface materials at the Gale crater revealed elevated concentrations of P2O5, SO3, Cl and Zn in soil compared to sand and active transportation processes for sand but not soil. The comprehensive chemical makeup of the Martian soil (inactive bedforms) and sand (active bedforms) is characterized by its basaltic nature, with enriched volatile elements such as sulphur, chlorine and zinc, and the presence of minerals like plagioclase, pyroxene and olivine due to the cohesive nature of inactive bedforms. Physical weathering and wind flow velocity play a pivotal role in the formation of different sedimentary bodies, impacting grain size distribution and mineralogy. The effect of dust-lifting on surface features is studied by analysing Perseverance-MEDA observations at the Jezero crater to understand the short-term changes in the bedform. These events are found to involve the redistribution of only a small amount of materials and, thereby, changing surface features on Mars over a short period. To detect the bedform migration in the Pasteur crater, several HiRISE images acquired over different time intervals were used. The changes in the ripple crest (~0.29–1.18 m/Earth year) and dune slip face suggest new grain flow events. In the Pasteur crater, extensive changes in sand deposits near the dunes signify a widespread bedform migration. The stronger north-westerly and north-easterly winds dominate these changes. Thus, the bedform migration in the three tropical craters exhibits significant variability driven by localized aeolian processes. This variability is crucial for understanding Mars' geological history, current surface dynamics and eventually, helps in planning future missions.
CONFLICT OF INTEREST STATEMENT
The authors do not have any known competing interests concerning financial, non-financial or personal aspects.
Open Research
DATA AVAILABILITY STATEMENT
The datasets used in the study are publicly available. The sand grain distribution data was taken from the article by Weitz et al. (2018), and the data is publicly available at https://figshare.com/articles/dataset/Grain_Sizes/16622854. The HiRISE RDRs used for this study are freely accessible at the University of Arizona website at https://www.uahirise.org/. The MEDA and APXS datasets are publicly available in the NASA PDS.
Supporting Information
| Filename | Description |
|---|---|
| esp6013-sup-0001-Supplementary_File.docWord document, 14.7 MB |
Figure S1. Context map of the Gale Crater (a), Jezero Crater (b) and Pasteur Crater (c). Figure S2. MAHLI images used in the study: (a) Rocknest, (b) Barker, (c) Kibnas, (d) Barby, (e) Flume Ridge, (f) Enchanted Island, (g) Thomas Little Toes, (h) Goatfell, (i) Gairsay, (j) Ellon, (k) Nairn, (l) Skipness and (m) Traquair. Figure S3. APXS measurement on Sol 531 with some of the major peaks labelled. Figure S4. Schematic diagram for bedform stability (Adopted from https://www.chegg.com/flashcards/sedimentary-petrology-midterm-55522a92-fb40-40dc-9a77-762868ea8d4e/deck) Figure S5. Wind speed variation corresponding to the considered events: (a) Sol 57, 10.58.32 LTST, (b) Sol 57, 12.38.52 LTST, (c) Sol 82, 12.04.41 LTST, (d) Sol 166, 13.05.33 LTST, (e) Sol 211, 12.00.17 LTST, (f) Sol 211, 12.20.45 LTST, (g) Sol 211, 13.24.03 LTST, (h) Sol 311, 12.17.37 LTST and (i) Sol 327, 13.04.40 LTST. Here, 0 indicates the time of the lowest pressure for the vortex activity and LTST indicates the local true solar time. Figure S6. Wind direction variation corresponding to the considered events: (a) Sol 57, 10.58.32 LTST, (b) Sol 57, 12.38.52 LTST, (c) Sol 82, 12.04.41 LTST, (d) Sol 166, 13.05.33 LTST, (e) Sol 211, 12.00.17 LTST, (f) Sol 211, 12.20.45 LTST, (g) Sol 211, 13.24.03 LTST, (h) Sol 311, 12.17.37 LTST and (i) Sol 327, 13.04.40 LTST. Here, 0 indicates the time of the lowest pressure for the vortex activity and LTST indicates the local true solar time. Figure S7. Variation of air temperature at 40 m elevation corresponding to the nine events considered in the study.: (a) Sol 57, 10.58.32 LTST, (b) Sol 57, 12.38.52 LTST, (c) Sol 82, 12.04.41 LTST, (d) Sol 166, 13.05.33 LTST, (e) Sol 211, 12.00.17 LTST, (f) Sol 211, 12.20.45 LTST, (g) Sol 211, 13.24.03 LTST, (h) Sol 311, 12.17.37 LTST and (i) Sol 327, 13.04.40 LTST. Here, 0 indicates the time of the lowest pressure for the vortex activity and LTST indicates the local true solar time. Figure S8. Variation of surface temperature corresponding to the considered events: (a) Sol 57, 10.58.32 LTST, (b) Sol 57, 12.38.52 LTST, (c) Sol 82, 12.04.41 LTST, (d) Sol 166, 13.05.33 LTST, (e) Sol 211, 12.00.17 LTST, (f) Sol 211, 12.20.45 LTST, (g) Sol 211, 13.24.03 LTST, (h) Sol 311, 12.17.37 LTST and (i) Sol 327, 13.04.40 LTST. Here, 0 indicates the time of the lowest pressure for the vortex activity and LTST indicates the local true solar time. Figure S9. Variation of reflected shortwave radiation corresponding to the considered events: (a) Sol 57, 10.58.32 LTST, (b) Sol 57, 12.38.52 LTST, (c) Sol 82, 12.04.41 LTST, (d) Sol 166, 13.05.33 LTST, (e) Sol 211, 12.00.17 LTST, (f) Sol 211, 12.20.45 LTST, (g) Sol 211, 13.24.03 LTST, (h) Sol 311, 12.17.37 LTST and (i) Sol 327, 13.04.40 LTST. Here, 0 indicates the time of the lowest pressure for the vortex activity and LTST indicates the local true solar time. Figure S10. Variation of downward longwave radiation corresponding to the considered events: (a) Sol 57, 10.58.32 LTST, (b) Sol 57, 12.38.52 LTST, (c) Sol 82, 12.04.41 LTST, (d) Sol 166, 13.05.33 LTST, (e) Sol 211, 12.00.17 LTST, (f) Sol 211, 12.20.45 LTST, (g) Sol 211, 13.24.03 LTST, (h) Sol 311, 12.17.37 LTST and (i) Sol 327, 13.04.40 LTST. Here, 0 indicates the time of the lowest pressure for the vortex activity and LTST indicates the local true solar time. Figure S11. The presence of a large number of rocks in the field of view of the Perseverance rover on Sol 211 visualized through the left Mastcam-Z images acquired at 11:58:52 local time (a) and 16:50:00 local time (b). Figure S12. Redistribution of finer particles at Jezero crater before the dust devil activity on Sol 298 (a), and after the activity on Sol 320 (b). Figure S13. Context illustration of the dune field inside the Pasteur crater used for the bedform migration analysis. Figure S14. Context illustration of the locations inside the Pasteur crater used for the black sand movement analysis. |
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