| タイトル |
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en
Scenarios for the formation of Chasma Boreale, Mars
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| 作成者 |
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| アクセス権 |
open access |
| 主題 |
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Other
en
Mars
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Other
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Polar cap
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Other
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Chasma Boreale
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Other
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Geothermal heat flux
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Other
is
Jökulhlaup
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NDC
445
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| 内容注記 |
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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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| 出版者 |
en
Academic Press
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| 日付 |
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| 言語 |
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| 資源タイプ |
journal article |
| 出版タイプ |
AM |
| 資源識別子 |
HDL
http://hdl.handle.net/2115/34403
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| 関連 |
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isVersionOf
DOI
https://doi.org/10.1016/j.icarus.2007.10.020
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| 収録誌情報 |
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PISSN
0019-1035
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NCID
AA00224921
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en
Icarus
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巻196
号2
開始ページ359
終了ページ367
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| ファイル |
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| コンテンツ更新日時 |
2023-07-26 |
