Permafrost on Mars: distribution, formation, and geological role
The morphology of channels, valleys, chaotic and fretted terrains and many smaller features on Mars is consistent with the hypothesis that localized deterioration of thick layers of ice-rich permafrost was a dominant geologic process on the Martian surface. Such ground ice deterioration gave rise to...
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ftnasantrs:oai:casi.ntrs.nasa.gov:19840015438 2023-05-15T16:36:49+02:00 Permafrost on Mars: distribution, formation, and geological role Nummedal, D. Unclassified, Unlimited, Publicly available Apr 1, 1984 http://ntrs.nasa.gov/search.jsp?R=19840015438 unknown http://ntrs.nasa.gov/search.jsp?R=19840015438 Accession ID: 84N23506 No Copyright CASI 91 NASA. Washington Rept. of Planetary Geol. Programs; p 209-211 1984 ftnasantrs 2012-02-15T15:41:40Z The morphology of channels, valleys, chaotic and fretted terrains and many smaller features on Mars is consistent with the hypothesis that localized deterioration of thick layers of ice-rich permafrost was a dominant geologic process on the Martian surface. Such ground ice deterioration gave rise to large-scale mass movement, including sliding, slumping and sediment gravity flowage, perhaps also catastropic floods. In contrast to Earth, such mass movement processes on Mars lack effective competition from erosion by surface runoff. Therefore, Martian features due to mass movement grew to reach immense size without being greatly modified by secondary erosional processes. The Viking Mission to Mars in 1976 provided adequate measurements of the relevant physical parameters to constrain models for Martian permafrost. Other/Unknown Material Ice permafrost NASA Technical Reports Server (NTRS) |
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NASA Technical Reports Server (NTRS) |
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ftnasantrs |
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unknown |
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91 |
spellingShingle |
91 Nummedal, D. Permafrost on Mars: distribution, formation, and geological role |
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91 |
description |
The morphology of channels, valleys, chaotic and fretted terrains and many smaller features on Mars is consistent with the hypothesis that localized deterioration of thick layers of ice-rich permafrost was a dominant geologic process on the Martian surface. Such ground ice deterioration gave rise to large-scale mass movement, including sliding, slumping and sediment gravity flowage, perhaps also catastropic floods. In contrast to Earth, such mass movement processes on Mars lack effective competition from erosion by surface runoff. Therefore, Martian features due to mass movement grew to reach immense size without being greatly modified by secondary erosional processes. The Viking Mission to Mars in 1976 provided adequate measurements of the relevant physical parameters to constrain models for Martian permafrost. |
format |
Other/Unknown Material |
author |
Nummedal, D. |
author_facet |
Nummedal, D. |
author_sort |
Nummedal, D. |
title |
Permafrost on Mars: distribution, formation, and geological role |
title_short |
Permafrost on Mars: distribution, formation, and geological role |
title_full |
Permafrost on Mars: distribution, formation, and geological role |
title_fullStr |
Permafrost on Mars: distribution, formation, and geological role |
title_full_unstemmed |
Permafrost on Mars: distribution, formation, and geological role |
title_sort |
permafrost on mars: distribution, formation, and geological role |
publishDate |
1984 |
url |
http://ntrs.nasa.gov/search.jsp?R=19840015438 |
op_coverage |
Unclassified, Unlimited, Publicly available |
genre |
Ice permafrost |
genre_facet |
Ice permafrost |
op_source |
CASI |
op_relation |
http://ntrs.nasa.gov/search.jsp?R=19840015438 Accession ID: 84N23506 |
op_rights |
No Copyright |
_version_ |
1766027148540248064 |