OMEGA/Mars Express: A new martian atmospheric dust hunter
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arXiv
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| Format: | Preprint |
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2025
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| _version_ | 1866909510709280768 |
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| author | Leseigneur, Yann Vincendon, Mathieu |
| author_facet | Leseigneur, Yann Vincendon, Mathieu |
| contents | While dust is a key parameter of Mars climate, its behaviour from one year to the next can appear erratic. This variability is notably related to Global Dust Storms (GDS) which occur only certain years with different onset, duration and intensity. The interannual variabilities of the dust cycle may notably explain some characteristics of Recurring Slope Lineae (RSL), slope flows once thought to be caused by liquid water. Long-term monitoring of dust dynamics is thus required to better understand surface-atmosphere dust exchanges on Mars. Here we present a new method to detect atmospheric dust as a function of space and time in the OMEGA Near-InfraRed (NIR) dataset. This dataset covers more than three Martian years; it includes the 2007 GDS which seasonality differs from the preceding (2001) and later (2018) GDS. The method is based on the decrease of the atmospheric optical path caused by dust, that can be measured by OMEGA with the 2 $μ$m CO$_2$ absorption band. This measure is converted to a 0.9 $μ$m NIR dust optical depth using notably comparisons with Mars Exploration Rovers measurements. We derive dust optical depth maps and comment on the variability of the dust seasonal cycle before, during and after the 2007 GDS. We also compare OMEGA NIR optical depths to Thermal InfraRed (TIR) ones derived by other studies. We found a NIR/TIR dust extinction optical depth ratio of 1.8 on average, with some variations notably related to dust particle size. Finally, we show in the northern hemisphere that atmospheric dust and RSL activity is correlated. This may indicate that dust lifting or transport mechanisms working at regional scale also participate to local RSL activity. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2502_18329 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | OMEGA/Mars Express: A new martian atmospheric dust hunter Leseigneur, Yann Vincendon, Mathieu Earth and Planetary Astrophysics Instrumentation and Methods for Astrophysics While dust is a key parameter of Mars climate, its behaviour from one year to the next can appear erratic. This variability is notably related to Global Dust Storms (GDS) which occur only certain years with different onset, duration and intensity. The interannual variabilities of the dust cycle may notably explain some characteristics of Recurring Slope Lineae (RSL), slope flows once thought to be caused by liquid water. Long-term monitoring of dust dynamics is thus required to better understand surface-atmosphere dust exchanges on Mars. Here we present a new method to detect atmospheric dust as a function of space and time in the OMEGA Near-InfraRed (NIR) dataset. This dataset covers more than three Martian years; it includes the 2007 GDS which seasonality differs from the preceding (2001) and later (2018) GDS. The method is based on the decrease of the atmospheric optical path caused by dust, that can be measured by OMEGA with the 2 $μ$m CO$_2$ absorption band. This measure is converted to a 0.9 $μ$m NIR dust optical depth using notably comparisons with Mars Exploration Rovers measurements. We derive dust optical depth maps and comment on the variability of the dust seasonal cycle before, during and after the 2007 GDS. We also compare OMEGA NIR optical depths to Thermal InfraRed (TIR) ones derived by other studies. We found a NIR/TIR dust extinction optical depth ratio of 1.8 on average, with some variations notably related to dust particle size. Finally, we show in the northern hemisphere that atmospheric dust and RSL activity is correlated. This may indicate that dust lifting or transport mechanisms working at regional scale also participate to local RSL activity. |
| title | OMEGA/Mars Express: A new martian atmospheric dust hunter |
| topic | Earth and Planetary Astrophysics Instrumentation and Methods for Astrophysics |
| url | https://arxiv.org/abs/2502.18329 |