High-resolution subsurface water-ice distributions on Mars
Theoretical models indicate that water ice is stable in the shallow subsurface (depths of
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| Veröffentlicht in: | Nature 2007-05, Vol.447 (7140), p.64-67 |
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| creator | Bandfield, Joshua L |
| description | Theoretical models indicate that water ice is stable in the shallow subsurface (depths of |
| doi_str_mv | 10.1038/nature05781 |
| format | Article |
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These models have been mainly supported by the observed presence of large concentrations of hydrogen detected by the Gamma Ray Spectrometer suite of instruments on the Mars Odyssey spacecraft. The models and measurements are consistent with a water-ice table that steadily increases in depth with decreasing latitude. More detailed modelling has predicted that the depth at which water ice is stable can be highly variable, owing to local surface heterogeneities such as rocks and slopes, and the thermal inertia of the ground cover. Measurements have, however, been limited to the footprint (several hundred kilometres) of the Gamma Ray Spectrometer suite, preventing the observations from documenting more detailed water-ice distributions. Here I show that by observing the seasonal temperature response of the martian surface with the Thermal Emission Imaging System on the Mars Odyssey spacecraft, it is possible to observe such heterogeneities at subkilometre scale. These observations show significant regional and local water-ice depth variability, and, in some cases, support distributions in the subsurface predicted by atmospheric exchange and vapour diffusion models. The presence of water ice where it follows the depth of stability under current climatic conditions implies an active martian water cycle that responds to orbit-driven climate cycles. Several regions also have apparent deviations from the theoretical stability level, indicating that additional factors influence the ice-table depth. The high-resolution measurements show that the depth to the water-ice table is highly variable within the potential Phoenix spacecraft landing ellipses, and is likely to be variable at scales that may be sampled by the spacecraft.</description><identifier>ISSN: 0028-0836</identifier><identifier>EISSN: 1476-4687</identifier><identifier>EISSN: 1476-4679</identifier><identifier>DOI: 10.1038/nature05781</identifier><identifier>PMID: 17476262</identifier><identifier>CODEN: NATUAS</identifier><language>eng</language><publisher>London: Nature Publishing Group UK</publisher><subject>Astronomy ; Climatic conditions ; Cosmochemistry. Extraterrestrial geology ; Earth sciences ; Earth, ocean, space ; Emissions ; Exact sciences and technology ; Extraterrestrial Environment - chemistry ; Extraterrestrial geology ; Gamma rays ; Ground cover ; Humanities and Social Sciences ; Hydrologic cycle ; Ice ; Ice - analysis ; Latitude ; letter ; Mars ; multidisciplinary ; Rocks ; Science ; Science (multidisciplinary) ; Spacecraft ; Subsurface water ; Temperature ; Theory ; Water - analysis ; Water depth</subject><ispartof>Nature, 2007-05, Vol.447 (7140), p.64-67</ispartof><rights>Springer Nature Limited 2007</rights><rights>2007 INIST-CNRS</rights><rights>COPYRIGHT 2007 Nature Publishing Group</rights><rights>Copyright Nature Publishing Group May 3, 2007</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-a764t-f01fafbcd45ecbd7c10c9d90dc7c07379ec554d4d813ba55b4296126555f732b3</citedby><cites>FETCH-LOGICAL-a764t-f01fafbcd45ecbd7c10c9d90dc7c07379ec554d4d813ba55b4296126555f732b3</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>315,781,785,2728,27926,27927</link.rule.ids><backlink>$$Uhttp://pascal-francis.inist.fr/vibad/index.php?action=getRecordDetail&idt=18699944$$DView record in Pascal Francis$$Hfree_for_read</backlink><backlink>$$Uhttps://www.ncbi.nlm.nih.gov/pubmed/17476262$$D View this record in MEDLINE/PubMed$$Hfree_for_read</backlink></links><search><creatorcontrib>Bandfield, Joshua L</creatorcontrib><title>High-resolution subsurface water-ice distributions on Mars</title><title>Nature</title><addtitle>Nature</addtitle><addtitle>Nature</addtitle><description>Theoretical models indicate that water ice is stable in the shallow subsurface (depths of <1-2 m) of Mars at high latitudes. These models have been mainly supported by the observed presence of large concentrations of hydrogen detected by the Gamma Ray Spectrometer suite of instruments on the Mars Odyssey spacecraft. The models and measurements are consistent with a water-ice table that steadily increases in depth with decreasing latitude. More detailed modelling has predicted that the depth at which water ice is stable can be highly variable, owing to local surface heterogeneities such as rocks and slopes, and the thermal inertia of the ground cover. Measurements have, however, been limited to the footprint (several hundred kilometres) of the Gamma Ray Spectrometer suite, preventing the observations from documenting more detailed water-ice distributions. Here I show that by observing the seasonal temperature response of the martian surface with the Thermal Emission Imaging System on the Mars Odyssey spacecraft, it is possible to observe such heterogeneities at subkilometre scale. These observations show significant regional and local water-ice depth variability, and, in some cases, support distributions in the subsurface predicted by atmospheric exchange and vapour diffusion models. The presence of water ice where it follows the depth of stability under current climatic conditions implies an active martian water cycle that responds to orbit-driven climate cycles. Several regions also have apparent deviations from the theoretical stability level, indicating that additional factors influence the ice-table depth. The high-resolution measurements show that the depth to the water-ice table is highly variable within the potential Phoenix spacecraft landing ellipses, and is likely to be variable at scales that may be sampled by the spacecraft.</description><subject>Astronomy</subject><subject>Climatic conditions</subject><subject>Cosmochemistry. 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Academic</collection><jtitle>Nature</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Bandfield, Joshua L</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>High-resolution subsurface water-ice distributions on Mars</atitle><jtitle>Nature</jtitle><stitle>Nature</stitle><addtitle>Nature</addtitle><date>2007-05-03</date><risdate>2007</risdate><volume>447</volume><issue>7140</issue><spage>64</spage><epage>67</epage><pages>64-67</pages><issn>0028-0836</issn><eissn>1476-4687</eissn><eissn>1476-4679</eissn><coden>NATUAS</coden><abstract>Theoretical models indicate that water ice is stable in the shallow subsurface (depths of <1-2 m) of Mars at high latitudes. These models have been mainly supported by the observed presence of large concentrations of hydrogen detected by the Gamma Ray Spectrometer suite of instruments on the Mars Odyssey spacecraft. The models and measurements are consistent with a water-ice table that steadily increases in depth with decreasing latitude. More detailed modelling has predicted that the depth at which water ice is stable can be highly variable, owing to local surface heterogeneities such as rocks and slopes, and the thermal inertia of the ground cover. Measurements have, however, been limited to the footprint (several hundred kilometres) of the Gamma Ray Spectrometer suite, preventing the observations from documenting more detailed water-ice distributions. Here I show that by observing the seasonal temperature response of the martian surface with the Thermal Emission Imaging System on the Mars Odyssey spacecraft, it is possible to observe such heterogeneities at subkilometre scale. These observations show significant regional and local water-ice depth variability, and, in some cases, support distributions in the subsurface predicted by atmospheric exchange and vapour diffusion models. The presence of water ice where it follows the depth of stability under current climatic conditions implies an active martian water cycle that responds to orbit-driven climate cycles. Several regions also have apparent deviations from the theoretical stability level, indicating that additional factors influence the ice-table depth. The high-resolution measurements show that the depth to the water-ice table is highly variable within the potential Phoenix spacecraft landing ellipses, and is likely to be variable at scales that may be sampled by the spacecraft.</abstract><cop>London</cop><pub>Nature Publishing Group UK</pub><pmid>17476262</pmid><doi>10.1038/nature05781</doi><tpages>4</tpages></addata></record> |
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| subjects | Astronomy Climatic conditions Cosmochemistry. Extraterrestrial geology Earth sciences Earth, ocean, space Emissions Exact sciences and technology Extraterrestrial Environment - chemistry Extraterrestrial geology Gamma rays Ground cover Humanities and Social Sciences Hydrologic cycle Ice Ice - analysis Latitude letter Mars multidisciplinary Rocks Science Science (multidisciplinary) Spacecraft Subsurface water Temperature Theory Water - analysis Water depth |
| title | High-resolution subsurface water-ice distributions on Mars |
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