Martian north polar cap summer water cycle
A key outstanding question in Martian science is 'are the polar caps gaining or losing mass and what are the implications for past, current and future climate?' To address this question, we use observations from the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) of the north...
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ftdatacite:10.48550/arxiv.1605.03487 2023-05-15T18:22:58+02:00 Martian north polar cap summer water cycle Brown, Adrian J. Calvin, Wendy M. Becerra, Patricio Byrne, Shane 2016 https://dx.doi.org/10.48550/arxiv.1605.03487 https://arxiv.org/abs/1605.03487 unknown arXiv https://dx.doi.org/10.1016/j.icarus.2016.05.007 arXiv.org perpetual, non-exclusive license http://arxiv.org/licenses/nonexclusive-distrib/1.0/ Earth and Planetary Astrophysics astro-ph.EP FOS Physical sciences article-journal Article ScholarlyArticle Text 2016 ftdatacite https://doi.org/10.48550/arxiv.1605.03487 https://doi.org/10.1016/j.icarus.2016.05.007 2022-04-01T11:34:18Z A key outstanding question in Martian science is 'are the polar caps gaining or losing mass and what are the implications for past, current and future climate?' To address this question, we use observations from the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) of the north polar cap during late summer for multiple Martian years, to monitor the summertime water cycle in order to place quantitative limits on the amount of water ice deposited and sublimed in late summer. We establish here for the first time the summer cycle of water ice absorption band signatures on the north polar cap. We show that in a key region in the interior of the north polar cap, the absorption band depths grow until Ls=120, when they begin to shrink, until they are obscured at the end of summer by the north polar hood. This behavior is transferable over the entire north polar cap, where in late summer regions 'flip' from being net sublimating into net condensation mode. This transition or 'mode flip' happens earlier for regions closer to the pole, and later for regions close to the periphery of the cap. The observations and calculations presented herein estimate that on average a water ice layer ~70 microns thick is deposited during the Ls=135-164 period. This is far larger than the results of deposition on the south pole during summer, where an average layer 0.6-6 microns deep has been estimated by Brown et al. (2014). : This article is closely related and draws from arXiv:1501.02040 Text South pole DataCite Metadata Store (German National Library of Science and Technology) South Pole |
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Earth and Planetary Astrophysics astro-ph.EP FOS Physical sciences |
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Earth and Planetary Astrophysics astro-ph.EP FOS Physical sciences Brown, Adrian J. Calvin, Wendy M. Becerra, Patricio Byrne, Shane Martian north polar cap summer water cycle |
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Earth and Planetary Astrophysics astro-ph.EP FOS Physical sciences |
description |
A key outstanding question in Martian science is 'are the polar caps gaining or losing mass and what are the implications for past, current and future climate?' To address this question, we use observations from the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) of the north polar cap during late summer for multiple Martian years, to monitor the summertime water cycle in order to place quantitative limits on the amount of water ice deposited and sublimed in late summer. We establish here for the first time the summer cycle of water ice absorption band signatures on the north polar cap. We show that in a key region in the interior of the north polar cap, the absorption band depths grow until Ls=120, when they begin to shrink, until they are obscured at the end of summer by the north polar hood. This behavior is transferable over the entire north polar cap, where in late summer regions 'flip' from being net sublimating into net condensation mode. This transition or 'mode flip' happens earlier for regions closer to the pole, and later for regions close to the periphery of the cap. The observations and calculations presented herein estimate that on average a water ice layer ~70 microns thick is deposited during the Ls=135-164 period. This is far larger than the results of deposition on the south pole during summer, where an average layer 0.6-6 microns deep has been estimated by Brown et al. (2014). : This article is closely related and draws from arXiv:1501.02040 |
format |
Text |
author |
Brown, Adrian J. Calvin, Wendy M. Becerra, Patricio Byrne, Shane |
author_facet |
Brown, Adrian J. Calvin, Wendy M. Becerra, Patricio Byrne, Shane |
author_sort |
Brown, Adrian J. |
title |
Martian north polar cap summer water cycle |
title_short |
Martian north polar cap summer water cycle |
title_full |
Martian north polar cap summer water cycle |
title_fullStr |
Martian north polar cap summer water cycle |
title_full_unstemmed |
Martian north polar cap summer water cycle |
title_sort |
martian north polar cap summer water cycle |
publisher |
arXiv |
publishDate |
2016 |
url |
https://dx.doi.org/10.48550/arxiv.1605.03487 https://arxiv.org/abs/1605.03487 |
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South Pole |
geographic_facet |
South Pole |
genre |
South pole |
genre_facet |
South pole |
op_relation |
https://dx.doi.org/10.1016/j.icarus.2016.05.007 |
op_rights |
arXiv.org perpetual, non-exclusive license http://arxiv.org/licenses/nonexclusive-distrib/1.0/ |
op_doi |
https://doi.org/10.48550/arxiv.1605.03487 https://doi.org/10.1016/j.icarus.2016.05.007 |
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1766202387286982656 |