| Title |
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en
Scenarios for the formation of Chasma Boreale, Mars
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| Creator |
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| Accessrights |
open access |
| Subject |
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Other
en
Mars
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Other
en
Polar cap
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Other
en
Chasma Boreale
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Other
en
Geothermal heat flux
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Other
is
Jökulhlaup
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NDC
445
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| Description |
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Abstract
en
The Martian polar caps feature large chasmata and smaller trough systems which have no counterpart in terrestrial ice sheets. Chasma Boreale cuts about 500 km into the western part of the north-polar cap, is up to 100 km wide and up to 2 km deep. One possible formation mechanism is by a temporary heat source under the ice due to tectonothermal or volcanic activity, which melts the ice from below. It is demonstrated by model simulations that this process is feasible, a moderately increased heat flux of 0.5–1Wm−2, sustained over at least tens of thousands of years, producing a topographic depression which resembles the real chasma. Associated meltwater discharge rates are small (< 1km3 a−1), but can exceed 10km3 a−1 if a stronger heat flux of 10Wm−2 is assumed. Local ice-flow velocities during the process of chasma formation can exceed 1ma−1 at the head and scarps of the chasma. However, if the thermal anomaly shuts down, glacial flow quickly decreases, so that the chasma can stay open for an indefinite amount of time without an ongoing, sustaining process under the climate conditions of the most recent millions of years.
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| Publisher |
en
Academic Press
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| Date |
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| Language |
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| Resource Type |
journal article |
| Version Type |
AM |
| Identifier |
HDL
http://hdl.handle.net/2115/34403
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| Relation |
-
isVersionOf
DOI
https://doi.org/10.1016/j.icarus.2007.10.020
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| Journal |
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-
PISSN
0019-1035
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NCID
AA00224921
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en
Icarus
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Volume Number196
Issue Number2
Page Start359
Page End367
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| File |
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| Oaidate |
2023-07-26 |
