Pitted rock surfaces on Mars: A mechanism of formation by transient melting of snow and ice
[1] Pits in rocks on the surface of Mars have been observed at several locations. Similar pits are observed in rocks in the Mars‐like hyperarid, hypothermal stable upland zone of the Antarctic Dry Valleys; these form by very localized chemical weathering due to transient melting of small amounts of...
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ftciteseerx:oai:CiteSeerX.psu:10.1.1.653.9526 2023-05-15T14:03:18+02:00 Pitted rock surfaces on Mars: A mechanism of formation by transient melting of snow and ice James W. Head Mikhail A. Kreslavsky David R. Marchant The Pennsylvania State University CiteSeerX Archives application/pdf http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.653.9526 http://planetary.brown.edu/pdfs/3622.pdf en eng http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.653.9526 http://planetary.brown.edu/pdfs/3622.pdf Metadata may be used without restrictions as long as the oai identifier remains attached to it. http://planetary.brown.edu/pdfs/3622.pdf text ftciteseerx 2016-01-08T16:31:30Z [1] Pits in rocks on the surface of Mars have been observed at several locations. Similar pits are observed in rocks in the Mars‐like hyperarid, hypothermal stable upland zone of the Antarctic Dry Valleys; these form by very localized chemical weathering due to transient melting of small amounts of snow on dark dolerite boulders preferentially heated above the melting point of water by sunlight. We examine the conditions under which a similar process might explain the pitted rocks seen on the surface of Mars (rock surface temperatures above the melting point; atmospheric pressure exceeding the triple point pressure of H2O; an available source of solid water to melt). We find that on Mars today each of these conditions is met locally and regionally, but that they do not occur together in such a way as to meet the stringent requirements for this process to operate. In the geological past, however, conditions favoring this process are highly likely to have been met. For example, increases in atmospheric water vapor content (due, for example, to the loss of the south perennial polar CO2 cap) could favor the deposition of snow, which if collected on rocks heated to above the melting temperature during favorable conditions (e.g., perihelion), could cause melting and the type of locally enhanced chemical weathering that can cause pits. Even when these conditions are met, however, the variation in heating of different rock facets under Martian conditions means that different parts of the rock may weather at different times, consistent with the very low weathering rates observed on Mars. Furthermore, as is the case in the stable upland zone of the Antarctic Dry Valleys, pit formation by transient melting of small amounts of snow readily occurs in the absence of subsurface active layer cryoturbation. Text Antarc* Antarctic Unknown Antarctic The Antarctic |
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[1] Pits in rocks on the surface of Mars have been observed at several locations. Similar pits are observed in rocks in the Mars‐like hyperarid, hypothermal stable upland zone of the Antarctic Dry Valleys; these form by very localized chemical weathering due to transient melting of small amounts of snow on dark dolerite boulders preferentially heated above the melting point of water by sunlight. We examine the conditions under which a similar process might explain the pitted rocks seen on the surface of Mars (rock surface temperatures above the melting point; atmospheric pressure exceeding the triple point pressure of H2O; an available source of solid water to melt). We find that on Mars today each of these conditions is met locally and regionally, but that they do not occur together in such a way as to meet the stringent requirements for this process to operate. In the geological past, however, conditions favoring this process are highly likely to have been met. For example, increases in atmospheric water vapor content (due, for example, to the loss of the south perennial polar CO2 cap) could favor the deposition of snow, which if collected on rocks heated to above the melting temperature during favorable conditions (e.g., perihelion), could cause melting and the type of locally enhanced chemical weathering that can cause pits. Even when these conditions are met, however, the variation in heating of different rock facets under Martian conditions means that different parts of the rock may weather at different times, consistent with the very low weathering rates observed on Mars. Furthermore, as is the case in the stable upland zone of the Antarctic Dry Valleys, pit formation by transient melting of small amounts of snow readily occurs in the absence of subsurface active layer cryoturbation. |
author2 |
The Pennsylvania State University CiteSeerX Archives |
format |
Text |
author |
James W. Head Mikhail A. Kreslavsky David R. Marchant |
spellingShingle |
James W. Head Mikhail A. Kreslavsky David R. Marchant Pitted rock surfaces on Mars: A mechanism of formation by transient melting of snow and ice |
author_facet |
James W. Head Mikhail A. Kreslavsky David R. Marchant |
author_sort |
James W. Head |
title |
Pitted rock surfaces on Mars: A mechanism of formation by transient melting of snow and ice |
title_short |
Pitted rock surfaces on Mars: A mechanism of formation by transient melting of snow and ice |
title_full |
Pitted rock surfaces on Mars: A mechanism of formation by transient melting of snow and ice |
title_fullStr |
Pitted rock surfaces on Mars: A mechanism of formation by transient melting of snow and ice |
title_full_unstemmed |
Pitted rock surfaces on Mars: A mechanism of formation by transient melting of snow and ice |
title_sort |
pitted rock surfaces on mars: a mechanism of formation by transient melting of snow and ice |
url |
http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.653.9526 http://planetary.brown.edu/pdfs/3622.pdf |
geographic |
Antarctic The Antarctic |
geographic_facet |
Antarctic The Antarctic |
genre |
Antarc* Antarctic |
genre_facet |
Antarc* Antarctic |
op_source |
http://planetary.brown.edu/pdfs/3622.pdf |
op_relation |
http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.653.9526 http://planetary.brown.edu/pdfs/3622.pdf |
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Metadata may be used without restrictions as long as the oai identifier remains attached to it. |
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1766273930713104384 |