Martian Volatiles: Isotopic Composition, Origin, and Evolution
Information about the composition of volatiles in the Martian atmosphere and interior derives from Viking spacecraft and ground-based measurements, and especially from measurements of volatiles trapped in Martian meteorites, which contain several distinct components. One volatile component, found in...
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| description | Information about the composition of volatiles in the Martian atmosphere and interior derives from Viking spacecraft and ground-based measurements, and especially from measurements of volatiles trapped in Martian meteorites, which contain several distinct components. One volatile component, found in impact glass in some shergottites, gives the most precise measurement to date of the composition of Martian atmospheric Ar, Kr, and Xe, and also contains significant amounts of atmospheric nitrogen showing elevated super(15)N/ super(14)N. Compared to Viking analyses, the super(36)Ar/ super(132)Xe and super(84)Kr/ super(132)Xe elemental ratios are larger in shergottites, the super(129)Xe/ super(132)Xe ratio is similar, and the super(40)Ar/ super(36)Ar and super(36)Ar/ super(38)Ar ratios are smaller. The isotopic composition of atmospheric Kr is very similar to solar Kr, whereas the isotopes of atmospheric Xe have been strongly mass fractionated in favor of heavier isotopes. The nakhlites and ALH84001 contain an atmospheric component elementally fractionated relative to the recent atmospheric component observed in shergottites. Several Martian meteorites also contain one or more Martian interior components that do not show the mass fractionation observed in atmospheric noble gases and nitrogen. The D/H ratio in the atmosphere is strongly mass fractionated, but meteorites contain a distinct Martian interior hydrogen component. The isotopic composition of Martian atmospheric carbon and oxygen have not been precisely measured, but these elements in meteorites appear to show much less variation in isotopic composition, presumably in part because of buffering of the atmospheric component by larger condensed reservoirs. However, differences in the oxygen isotopic composition between meteorite silicate minerals (on the one hand) and water and carbonates indicate a lack of recycling of these volatiles through the interior. Many models have been presented to explain the observed isotopic fractionation in Martian atmospheric N, H, and noble gases in terms of partial loss of the planetary atmosphere, either very early in Martian history, or over extended geological time. The number of variables in these models is large, and we cannot be certain of their detailed applicability. Evolutionary data based on the radiogenic isotopes (i.e., super(40)Ar/ super(36)Ar, super(129)Xe/ super(132)Xe, and super(136)Xe/ super(132)Xe ratios) are potentially important, but meteorite data do |
| doi_str_mv | 10.1023/A:1011974028370 |
| format | Article |
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One volatile component, found in impact glass in some shergottites, gives the most precise measurement to date of the composition of Martian atmospheric Ar, Kr, and Xe, and also contains significant amounts of atmospheric nitrogen showing elevated super(15)N/ super(14)N. Compared to Viking analyses, the super(36)Ar/ super(132)Xe and super(84)Kr/ super(132)Xe elemental ratios are larger in shergottites, the super(129)Xe/ super(132)Xe ratio is similar, and the super(40)Ar/ super(36)Ar and super(36)Ar/ super(38)Ar ratios are smaller. The isotopic composition of atmospheric Kr is very similar to solar Kr, whereas the isotopes of atmospheric Xe have been strongly mass fractionated in favor of heavier isotopes. The nakhlites and ALH84001 contain an atmospheric component elementally fractionated relative to the recent atmospheric component observed in shergottites. Several Martian meteorites also contain one or more Martian interior components that do not show the mass fractionation observed in atmospheric noble gases and nitrogen. The D/H ratio in the atmosphere is strongly mass fractionated, but meteorites contain a distinct Martian interior hydrogen component. The isotopic composition of Martian atmospheric carbon and oxygen have not been precisely measured, but these elements in meteorites appear to show much less variation in isotopic composition, presumably in part because of buffering of the atmospheric component by larger condensed reservoirs. However, differences in the oxygen isotopic composition between meteorite silicate minerals (on the one hand) and water and carbonates indicate a lack of recycling of these volatiles through the interior. Many models have been presented to explain the observed isotopic fractionation in Martian atmospheric N, H, and noble gases in terms of partial loss of the planetary atmosphere, either very early in Martian history, or over extended geological time. The number of variables in these models is large, and we cannot be certain of their detailed applicability. Evolutionary data based on the radiogenic isotopes (i.e., super(40)Ar/ super(36)Ar, super(129)Xe/ super(132)Xe, and super(136)Xe/ super(132)Xe ratios) are potentially important, but meteorite data do not yet permit their use in detailed chronologies. The sources of Mars' original volatiles are not well defined. Some Martian components require a solar-like isotopic composition, whereas volatiles other than the noble gases (C, N, and H sub(2)O) may have been largely contributed by a carbonaceous (or cometary) veneer late in planet formation. Also, carbonaceous material may have been the source of moderate amounts of water early in Martian history.</description><identifier>ISSN: 0038-6308</identifier><identifier>EISSN: 1572-9672</identifier><identifier>DOI: 10.1023/A:1011974028370</identifier><language>eng</language><publisher>Dordrecht: Springer Nature B.V</publisher><subject>Atmosphere ; Carbonates ; Fractionation ; Geological time ; Isotope fractionation ; Isotopes ; Mars ; Meteors & meteorites ; Nitrogen ; Ratios ; Spacecraft</subject><ispartof>Space science reviews, 2001-04, Vol.96 (1-4), p.425-458</ispartof><rights>Kluwer Academic Publishers 2001</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c386t-7e73d316b0b96ecef0496c60d763f0e5ffd81e218a4662ec379447787a7495c3</citedby></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,776,780,27901,27902</link.rule.ids></links><search><creatorcontrib>Bogard, D D</creatorcontrib><creatorcontrib>Clayton, R N</creatorcontrib><creatorcontrib>Marti, K</creatorcontrib><creatorcontrib>Owen, T</creatorcontrib><creatorcontrib>Turner, G</creatorcontrib><title>Martian Volatiles: Isotopic Composition, Origin, and Evolution</title><title>Space science reviews</title><description>Information about the composition of volatiles in the Martian atmosphere and interior derives from Viking spacecraft and ground-based measurements, and especially from measurements of volatiles trapped in Martian meteorites, which contain several distinct components. One volatile component, found in impact glass in some shergottites, gives the most precise measurement to date of the composition of Martian atmospheric Ar, Kr, and Xe, and also contains significant amounts of atmospheric nitrogen showing elevated super(15)N/ super(14)N. Compared to Viking analyses, the super(36)Ar/ super(132)Xe and super(84)Kr/ super(132)Xe elemental ratios are larger in shergottites, the super(129)Xe/ super(132)Xe ratio is similar, and the super(40)Ar/ super(36)Ar and super(36)Ar/ super(38)Ar ratios are smaller. The isotopic composition of atmospheric Kr is very similar to solar Kr, whereas the isotopes of atmospheric Xe have been strongly mass fractionated in favor of heavier isotopes. The nakhlites and ALH84001 contain an atmospheric component elementally fractionated relative to the recent atmospheric component observed in shergottites. Several Martian meteorites also contain one or more Martian interior components that do not show the mass fractionation observed in atmospheric noble gases and nitrogen. The D/H ratio in the atmosphere is strongly mass fractionated, but meteorites contain a distinct Martian interior hydrogen component. The isotopic composition of Martian atmospheric carbon and oxygen have not been precisely measured, but these elements in meteorites appear to show much less variation in isotopic composition, presumably in part because of buffering of the atmospheric component by larger condensed reservoirs. However, differences in the oxygen isotopic composition between meteorite silicate minerals (on the one hand) and water and carbonates indicate a lack of recycling of these volatiles through the interior. Many models have been presented to explain the observed isotopic fractionation in Martian atmospheric N, H, and noble gases in terms of partial loss of the planetary atmosphere, either very early in Martian history, or over extended geological time. The number of variables in these models is large, and we cannot be certain of their detailed applicability. Evolutionary data based on the radiogenic isotopes (i.e., super(40)Ar/ super(36)Ar, super(129)Xe/ super(132)Xe, and super(136)Xe/ super(132)Xe ratios) are potentially important, but meteorite data do not yet permit their use in detailed chronologies. The sources of Mars' original volatiles are not well defined. Some Martian components require a solar-like isotopic composition, whereas volatiles other than the noble gases (C, N, and H sub(2)O) may have been largely contributed by a carbonaceous (or cometary) veneer late in planet formation. Also, carbonaceous material may have been the source of moderate amounts of water early in Martian history.</description><subject>Atmosphere</subject><subject>Carbonates</subject><subject>Fractionation</subject><subject>Geological time</subject><subject>Isotope fractionation</subject><subject>Isotopes</subject><subject>Mars</subject><subject>Meteors & meteorites</subject><subject>Nitrogen</subject><subject>Ratios</subject><subject>Spacecraft</subject><issn>0038-6308</issn><issn>1572-9672</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2001</creationdate><recordtype>article</recordtype><sourceid>BENPR</sourceid><recordid>eNqFz81LAzEQBfAgCtbq2eviQS-uTj4n6UEopWqh0kvxWtJsVlK2m7rZ9e83oicPenow_HiPIeSSwh0Fxu-nEwqUGhTANEc4IiMqkZVGITsmIwCuS8VBn5KzlHYAFABxRB5ebNcH2xavsbF9aHyaFIsU-3gIrpjF_SGm0IfY3harLryFnLativlHbIav8zk5qW2T_MVPjsn6cb6ePZfL1dNiNl2WjmvVl-iRV5yqLWyN8s7XIIxyCipUvAYv67rS1DOqrVCKecfRCIGo0aIw0vExufmuPXTxffCp3-xDcr5pbOvjkDZGCskocpHl9Z-SKZ0dh38h1VKh4DLDq19wF4euzd9u8qCSuUvxT5hacTk</recordid><startdate>20010401</startdate><enddate>20010401</enddate><creator>Bogard, D D</creator><creator>Clayton, R N</creator><creator>Marti, K</creator><creator>Owen, T</creator><creator>Turner, G</creator><general>Springer Nature B.V</general><scope>3V.</scope><scope>7TG</scope><scope>7XB</scope><scope>88I</scope><scope>8FD</scope><scope>8FE</scope><scope>8FG</scope><scope>8FK</scope><scope>ABUWG</scope><scope>AEUYN</scope><scope>AFKRA</scope><scope>ARAPS</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>GNUQQ</scope><scope>H8D</scope><scope>HCIFZ</scope><scope>KL.</scope><scope>L7M</scope><scope>M2P</scope><scope>P5Z</scope><scope>P62</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>Q9U</scope></search><sort><creationdate>20010401</creationdate><title>Martian Volatiles: Isotopic Composition, Origin, and Evolution</title><author>Bogard, D D ; Clayton, R N ; Marti, K ; Owen, T ; Turner, G</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c386t-7e73d316b0b96ecef0496c60d763f0e5ffd81e218a4662ec379447787a7495c3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2001</creationdate><topic>Atmosphere</topic><topic>Carbonates</topic><topic>Fractionation</topic><topic>Geological time</topic><topic>Isotope fractionation</topic><topic>Isotopes</topic><topic>Mars</topic><topic>Meteors & meteorites</topic><topic>Nitrogen</topic><topic>Ratios</topic><topic>Spacecraft</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Bogard, D D</creatorcontrib><creatorcontrib>Clayton, R N</creatorcontrib><creatorcontrib>Marti, K</creatorcontrib><creatorcontrib>Owen, T</creatorcontrib><creatorcontrib>Turner, G</creatorcontrib><collection>ProQuest Central (Corporate)</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>ProQuest Central (purchase pre-March 2016)</collection><collection>Science Database (Alumni Edition)</collection><collection>Technology Research Database</collection><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>ProQuest Central (Alumni) (purchase pre-March 2016)</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest One Sustainability</collection><collection>ProQuest Central UK/Ireland</collection><collection>Advanced Technologies & Aerospace Collection</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>ProQuest Central Student</collection><collection>Aerospace Database</collection><collection>SciTech Premium Collection</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Science Database</collection><collection>Advanced Technologies & Aerospace Database</collection><collection>ProQuest Advanced Technologies & Aerospace Collection</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central Basic</collection><jtitle>Space science reviews</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Bogard, D D</au><au>Clayton, R N</au><au>Marti, K</au><au>Owen, T</au><au>Turner, G</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Martian Volatiles: Isotopic Composition, Origin, and Evolution</atitle><jtitle>Space science reviews</jtitle><date>2001-04-01</date><risdate>2001</risdate><volume>96</volume><issue>1-4</issue><spage>425</spage><epage>458</epage><pages>425-458</pages><issn>0038-6308</issn><eissn>1572-9672</eissn><abstract>Information about the composition of volatiles in the Martian atmosphere and interior derives from Viking spacecraft and ground-based measurements, and especially from measurements of volatiles trapped in Martian meteorites, which contain several distinct components. One volatile component, found in impact glass in some shergottites, gives the most precise measurement to date of the composition of Martian atmospheric Ar, Kr, and Xe, and also contains significant amounts of atmospheric nitrogen showing elevated super(15)N/ super(14)N. Compared to Viking analyses, the super(36)Ar/ super(132)Xe and super(84)Kr/ super(132)Xe elemental ratios are larger in shergottites, the super(129)Xe/ super(132)Xe ratio is similar, and the super(40)Ar/ super(36)Ar and super(36)Ar/ super(38)Ar ratios are smaller. The isotopic composition of atmospheric Kr is very similar to solar Kr, whereas the isotopes of atmospheric Xe have been strongly mass fractionated in favor of heavier isotopes. The nakhlites and ALH84001 contain an atmospheric component elementally fractionated relative to the recent atmospheric component observed in shergottites. Several Martian meteorites also contain one or more Martian interior components that do not show the mass fractionation observed in atmospheric noble gases and nitrogen. The D/H ratio in the atmosphere is strongly mass fractionated, but meteorites contain a distinct Martian interior hydrogen component. The isotopic composition of Martian atmospheric carbon and oxygen have not been precisely measured, but these elements in meteorites appear to show much less variation in isotopic composition, presumably in part because of buffering of the atmospheric component by larger condensed reservoirs. However, differences in the oxygen isotopic composition between meteorite silicate minerals (on the one hand) and water and carbonates indicate a lack of recycling of these volatiles through the interior. Many models have been presented to explain the observed isotopic fractionation in Martian atmospheric N, H, and noble gases in terms of partial loss of the planetary atmosphere, either very early in Martian history, or over extended geological time. The number of variables in these models is large, and we cannot be certain of their detailed applicability. Evolutionary data based on the radiogenic isotopes (i.e., super(40)Ar/ super(36)Ar, super(129)Xe/ super(132)Xe, and super(136)Xe/ super(132)Xe ratios) are potentially important, but meteorite data do not yet permit their use in detailed chronologies. The sources of Mars' original volatiles are not well defined. Some Martian components require a solar-like isotopic composition, whereas volatiles other than the noble gases (C, N, and H sub(2)O) may have been largely contributed by a carbonaceous (or cometary) veneer late in planet formation. Also, carbonaceous material may have been the source of moderate amounts of water early in Martian history.</abstract><cop>Dordrecht</cop><pub>Springer Nature B.V</pub><doi>10.1023/A:1011974028370</doi><tpages>34</tpages></addata></record> |
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| subjects | Atmosphere Carbonates Fractionation Geological time Isotope fractionation Isotopes Mars Meteors & meteorites Nitrogen Ratios Spacecraft |
| title | Martian Volatiles: Isotopic Composition, Origin, and Evolution |
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