The atmospheric circulation and dust activity in different orbital epochs on Mars
A general circulation model is used to evaluate changes to the circulation and dust transport in the martian atmosphere for a range of past orbital conditions. A dust transport scheme, including parameterized dust lifting, is incorporated within the model to enable passive or radiatively active dust...
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Online Access: | https://doi.org/10.1016/j.icarus.2004.10.023 https://ora.ox.ac.uk/objects/uuid:23ee77e0-5528-4a85-a8ef-e4fbc48bbf9b |
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ftuloxford:oai:ora.ox.ac.uk:uuid:23ee77e0-5528-4a85-a8ef-e4fbc48bbf9b 2023-05-15T16:38:21+02:00 The atmospheric circulation and dust activity in different orbital epochs on Mars Newman, C Lewis, SR Read, P 2016-07-28 https://doi.org/10.1016/j.icarus.2004.10.023 https://ora.ox.ac.uk/objects/uuid:23ee77e0-5528-4a85-a8ef-e4fbc48bbf9b eng eng doi:10.1016/j.icarus.2004.10.023 https://ora.ox.ac.uk/objects/uuid:23ee77e0-5528-4a85-a8ef-e4fbc48bbf9b https://doi.org/10.1016/j.icarus.2004.10.023 info:eu-repo/semantics/embargoedAccess Journal article 2016 ftuloxford https://doi.org/10.1016/j.icarus.2004.10.023 2022-06-28T20:07:55Z A general circulation model is used to evaluate changes to the circulation and dust transport in the martian atmosphere for a range of past orbital conditions. A dust transport scheme, including parameterized dust lifting, is incorporated within the model to enable passive or radiatively active dust transport. The focus is on changes which relate to surface features, as these may potentially be verified by observations. Obliquity variations have the largest impact, as they affect the latitudinal distribution of solar heating. At low obliquities permanent CO 2 ice caps form at both poles, lowering mean surface pressures. At higher obliquities, solar insolation peaks at higher summer latitudes near solstice, producing a stronger, broader meridional circulation and a larger seasonal CO 2 ice cap in winter. Near-surface winds associated with the main meridional circulation intensify and extend polewards, with changes in cap edge position also affecting the flow. Hence the model predicts significant changes in surface wind directions as well as magnitudes. Dust lifting by wind stress increases with obliquity as the meridional circulation and associated near-surface winds strengthen. If active dust transport is used, then lifting rates increase further in response to the larger atmospheric dust opacities (hence circulation) produced. Dust lifting by dust devils increases more gradually with obliquity, having a weaker link to the meridional circulation. The primary effect of varying eccentricity is to change the impact of varying the areocentric longitude of perihelion, l, which determines when the solar forcing is strongest. The atmospheric circulation is stronger when l aligns with solstice rather than equinox, and there is also a bias from the martian topography, resulting in the strongest circulations when perihelion is at northern winter solstice. Net dust accumulation depends on both lifting and deposition. Dust which has been well mixed within the atmosphere is deposited preferentially over high topography. For ... Article in Journal/Newspaper Ice cap ORA - Oxford University Research Archive Icarus 174 1 135 160 |
institution |
Open Polar |
collection |
ORA - Oxford University Research Archive |
op_collection_id |
ftuloxford |
language |
English |
description |
A general circulation model is used to evaluate changes to the circulation and dust transport in the martian atmosphere for a range of past orbital conditions. A dust transport scheme, including parameterized dust lifting, is incorporated within the model to enable passive or radiatively active dust transport. The focus is on changes which relate to surface features, as these may potentially be verified by observations. Obliquity variations have the largest impact, as they affect the latitudinal distribution of solar heating. At low obliquities permanent CO 2 ice caps form at both poles, lowering mean surface pressures. At higher obliquities, solar insolation peaks at higher summer latitudes near solstice, producing a stronger, broader meridional circulation and a larger seasonal CO 2 ice cap in winter. Near-surface winds associated with the main meridional circulation intensify and extend polewards, with changes in cap edge position also affecting the flow. Hence the model predicts significant changes in surface wind directions as well as magnitudes. Dust lifting by wind stress increases with obliquity as the meridional circulation and associated near-surface winds strengthen. If active dust transport is used, then lifting rates increase further in response to the larger atmospheric dust opacities (hence circulation) produced. Dust lifting by dust devils increases more gradually with obliquity, having a weaker link to the meridional circulation. The primary effect of varying eccentricity is to change the impact of varying the areocentric longitude of perihelion, l, which determines when the solar forcing is strongest. The atmospheric circulation is stronger when l aligns with solstice rather than equinox, and there is also a bias from the martian topography, resulting in the strongest circulations when perihelion is at northern winter solstice. Net dust accumulation depends on both lifting and deposition. Dust which has been well mixed within the atmosphere is deposited preferentially over high topography. For ... |
format |
Article in Journal/Newspaper |
author |
Newman, C Lewis, SR Read, P |
spellingShingle |
Newman, C Lewis, SR Read, P The atmospheric circulation and dust activity in different orbital epochs on Mars |
author_facet |
Newman, C Lewis, SR Read, P |
author_sort |
Newman, C |
title |
The atmospheric circulation and dust activity in different orbital epochs on Mars |
title_short |
The atmospheric circulation and dust activity in different orbital epochs on Mars |
title_full |
The atmospheric circulation and dust activity in different orbital epochs on Mars |
title_fullStr |
The atmospheric circulation and dust activity in different orbital epochs on Mars |
title_full_unstemmed |
The atmospheric circulation and dust activity in different orbital epochs on Mars |
title_sort |
atmospheric circulation and dust activity in different orbital epochs on mars |
publishDate |
2016 |
url |
https://doi.org/10.1016/j.icarus.2004.10.023 https://ora.ox.ac.uk/objects/uuid:23ee77e0-5528-4a85-a8ef-e4fbc48bbf9b |
genre |
Ice cap |
genre_facet |
Ice cap |
op_relation |
doi:10.1016/j.icarus.2004.10.023 https://ora.ox.ac.uk/objects/uuid:23ee77e0-5528-4a85-a8ef-e4fbc48bbf9b https://doi.org/10.1016/j.icarus.2004.10.023 |
op_rights |
info:eu-repo/semantics/embargoedAccess |
op_doi |
https://doi.org/10.1016/j.icarus.2004.10.023 |
container_title |
Icarus |
container_volume |
174 |
container_issue |
1 |
container_start_page |
135 |
op_container_end_page |
160 |
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1766028623626633216 |