Primitive olivine‐phyric shergottite NWA 5789: Petrography, mineral chemistry, and cooling history imply a magma similar to Yamato‐980459
Identifieur interne : 001B36 ( Istex/Corpus ); précédent : 001B35; suivant : 001B37Primitive olivine‐phyric shergottite NWA 5789: Petrography, mineral chemistry, and cooling history imply a magma similar to Yamato‐980459
Auteurs : Juliane Gross ; Allan H. Treiman ; Justin Filiberto ; Christopher D. K. HerdSource :
- Meteoritics & Planetary Science [ 1086-9379 ] ; 2011-01.
Abstract
Knowledge of Martian igneous basaltic compositions is crucial for constraining mantle evolution, including early differentiation and mantle convection. Primitive magmas provide direct information about their mantle source regions, but most Martian meteorites either contain cumulate olivine or crystallized from fractionated melts. The recently discovered Martian meteorite Northwest Africa (NWA) 5789 is an olivine‐phyric shergottite. NWA 5789 has special significance among the Martian meteorites because it appears to represent one of the most magnesian Martian magmas known, other than Yamato (Y) 980459. Its most magnesian olivine cores (Fo85) are in Mg‐Fe equilibrium with a magma of the bulk rock composition, suggesting that the bulk represents a magma composition. Based on the Al/Ti ratio of its pyroxenes, we infer that the rock began to crystallize at a high pressure consistent with conditions in Mars’ lower crust/upper mantle. It continued and completed its crystallization closer to the surface, where cooling was rapid and produced a mesostasis of radiating sprays of plagioclase and pyroxene. The mineralogy, petrology, mineral chemistry, and bulk rock composition of NWA 5789 are very similar to those of Y‐980459. The similarities between the two meteorites suggest that NWA 5789 (like Y‐980459) represents a primitive, mantle‐derived magma composition. They also suggest the possibility that NWA 5789 and Y‐980459 formed in the same lava flow. However, based on the mineralogy and texture of its mesostasis, NWA 5789 must have cooled more slowly than Y‐980459. NWA 5789 will help elucidate the igneous geology and geochemistry of Mars.
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DOI: 10.1111/j.1945-5100.2010.01152.x
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Treiman</name><affiliation><mods:affiliation>Lunar and Planetary Institute, 3600 Bay Area Boulevard, Houston, Texas 77058, USA</mods:affiliation></affiliation></author><author><name sortKey="Filiberto, Justin" sort="Filiberto, Justin" uniqKey="Filiberto J" first="Justin" last="Filiberto">Justin Filiberto</name><affiliation><mods:affiliation>Department of Earth Science MS‐126, Rice University, 6100 Main St., Houston, Texas 77005, USA</mods:affiliation></affiliation></author><author><name sortKey="Herd, Christopher D K" sort="Herd, Christopher D K" uniqKey="Herd C" first="Christopher D. K." last="Herd">Christopher D. K. 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Primitive magmas provide direct information about their mantle source regions, but most Martian meteorites either contain cumulate olivine or crystallized from fractionated melts. The recently discovered Martian meteorite Northwest Africa (NWA) 5789 is an olivine‐phyric shergottite. NWA 5789 has special significance among the Martian meteorites because it appears to represent one of the most magnesian Martian magmas known, other than Yamato (Y) 980459. Its most magnesian olivine cores (Fo85) are in Mg‐Fe equilibrium with a magma of the bulk rock composition, suggesting that the bulk represents a magma composition. Based on the Al/Ti ratio of its pyroxenes, we infer that the rock began to crystallize at a high pressure consistent with conditions in Mars’ lower crust/upper mantle. It continued and completed its crystallization closer to the surface, where cooling was rapid and produced a mesostasis of radiating sprays of plagioclase and pyroxene. The mineralogy, petrology, mineral chemistry, and bulk rock composition of NWA 5789 are very similar to those of Y‐980459. The similarities between the two meteorites suggest that NWA 5789 (like Y‐980459) represents a primitive, mantle‐derived magma composition. They also suggest the possibility that NWA 5789 and Y‐980459 formed in the same lava flow. However, based on the mineralogy and texture of its mesostasis, NWA 5789 must have cooled more slowly than Y‐980459. NWA 5789 will help elucidate the igneous geology and geochemistry of Mars.</div></front></TEI><istex><corpusName>wiley</corpusName><author><json:item><name>Juliane GROSS</name><affiliations><json:string>Lunar and Planetary Institute, 3600 Bay Area Boulevard, Houston, Texas 77058, USA</json:string></affiliations></json:item><json:item><name>Allan H. 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The mineralogy, petrology, mineral chemistry, and bulk rock composition of NWA 5789 are very similar to those of Y‐980459. The similarities between the two meteorites suggest that NWA 5789 (like Y‐980459) represents a primitive, mantle‐derived magma composition. They also suggest the possibility that NWA 5789 and Y‐980459 formed in the same lava flow. However, based on the mineralogy and texture of its mesostasis, NWA 5789 must have cooled more slowly than Y‐980459. 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E‐mail:</p></note><affiliation>Lunar and Planetary Institute, 3600 Bay Area Boulevard, Houston, Texas 77058, USA</affiliation></author><author xml:id="author-2"><persName><forename type="first">Allan H.</forename><surname>TREIMAN</surname></persName><affiliation>Lunar and Planetary Institute, 3600 Bay Area Boulevard, Houston, Texas 77058, USA</affiliation></author><author xml:id="author-3"><persName><forename type="first">Justin</forename><surname>FILIBERTO</surname></persName><affiliation>Department of Earth Science MS‐126, Rice University, 6100 Main St., Houston, Texas 77005, USA</affiliation></author><author xml:id="author-4"><persName><forename type="first">Christopher D. K.</forename><surname>HERD</surname></persName><affiliation>Department of Earth and Atmospheric Sciences, University of Alberta, Edmonton, Alberta T6G 2E3, Canada</affiliation></author></analytic><monogr><title level="j">Meteoritics & Planetary Science</title><idno type="pISSN">1086-9379</idno><idno type="eISSN">1945-5100</idno><idno type="DOI">10.1111/(ISSN)1945-5100</idno><imprint><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2011-01"></date><biblScope unit="volume">46</biblScope><biblScope unit="issue">1</biblScope><biblScope unit="page" from="116">116</biblScope><biblScope unit="page" to="133">133</biblScope></imprint></monogr><idno type="istex">0DE34CF31ED2C8BBEA689BE3AC0D74FFC6A96C78</idno><idno type="DOI">10.1111/j.1945-5100.2010.01152.x</idno><idno type="ArticleID">MAPS1152</idno></biblStruct></sourceDesc></fileDesc><profileDesc><creation><date>2011</date></creation><langUsage><language ident="en">en</language></langUsage><abstract xml:lang="en"><p>Knowledge of Martian igneous basaltic compositions is crucial for constraining mantle evolution, including early differentiation and mantle convection. Primitive magmas provide direct information about their mantle source regions, but most Martian meteorites either contain cumulate olivine or crystallized from fractionated melts. The recently discovered Martian meteorite Northwest Africa (NWA) 5789 is an olivine‐phyric shergottite. NWA 5789 has special significance among the Martian meteorites because it appears to represent one of the most magnesian Martian magmas known, other than Yamato (Y) 980459. Its most magnesian olivine cores (Fo85) are in Mg‐Fe equilibrium with a magma of the bulk rock composition, suggesting that the bulk represents a magma composition. Based on the Al/Ti ratio of its pyroxenes, we infer that the rock began to crystallize at a high pressure consistent with conditions in Mars’ lower crust/upper mantle. It continued and completed its crystallization closer to the surface, where cooling was rapid and produced a mesostasis of radiating sprays of plagioclase and pyroxene. The mineralogy, petrology, mineral chemistry, and bulk rock composition of NWA 5789 are very similar to those of Y‐980459. The similarities between the two meteorites suggest that NWA 5789 (like Y‐980459) represents a primitive, mantle‐derived magma composition. They also suggest the possibility that NWA 5789 and Y‐980459 formed in the same lava flow. However, based on the mineralogy and texture of its mesostasis, NWA 5789 must have cooled more slowly than Y‐980459. 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E‐mail: <email>gross@lpi.usra.edu</email></correspondenceTo><linkGroup><link type="toTypesetVersion" href="file:MAPS.MAPS1152.pdf"></link></linkGroup></publicationMeta><contentMeta><unparsedEditorialHistory>(Received 28 April 2010; revision accepted 30 September 2010)</unparsedEditorialHistory><countGroup><count type="figureTotal" number="13"></count><count type="tableTotal" number="6"></count></countGroup><titleGroup><title type="main">Primitive olivine‐phyric shergottite NWA 5789: Petrography, mineral chemistry, and cooling history imply a magma similar to Yamato‐980459</title><title type="shortAuthors">J. Gross et al.</title><title type="short">Primitive olivine‐phyric shergottite NWA 5789</title></titleGroup><creators><creator creatorRole="author" xml:id="cr1" affiliationRef="#a1" corresponding="yes"><personName><givenNames>Juliane</givenNames><familyName>GROSS</familyName></personName></creator><creator creatorRole="author" xml:id="cr2" affiliationRef="#a1"><personName><givenNames>Allan H.</givenNames><familyName>TREIMAN</familyName></personName></creator><creator creatorRole="author" xml:id="cr3" affiliationRef="#a2"><personName><givenNames>Justin</givenNames><familyName>FILIBERTO</familyName></personName></creator><creator creatorRole="author" xml:id="cr4" affiliationRef="#a3"><personName><givenNames>Christopher D. K.</givenNames><familyName>HERD</familyName></personName></creator></creators><affiliationGroup><affiliation xml:id="a1" countryCode="US"><unparsedAffiliation>Lunar and Planetary Institute, 3600 Bay Area Boulevard, Houston, Texas 77058, USA</unparsedAffiliation></affiliation><affiliation xml:id="a2" countryCode="US"><unparsedAffiliation>Department of Earth Science MS‐126, Rice University, 6100 Main St., Houston, Texas 77005, USA</unparsedAffiliation></affiliation><affiliation xml:id="a3" countryCode="CA"><unparsedAffiliation>Department of Earth and Atmospheric Sciences, University of Alberta, Edmonton, Alberta T6G 2E3, Canada</unparsedAffiliation></affiliation></affiliationGroup><supportingInformation><p><b>Table S1.</b> Microprobe analyses of olivine.</p><p><b>Table S2.</b> Microprobe analyses of pyroxene.</p><p><b>Table S3.</b> Microprobe analyses of plagioclase.</p><supportingInfoItem><mediaResource alt="supporting info item" href="urn-x:wiley:10869379:media:maps1152:MAPS_1152_sm_online-supplemental-olivine"></mediaResource><caption>Supporting info item</caption></supportingInfoItem><supportingInfoItem><mediaResource alt="supporting info item" href="urn-x:wiley:10869379:media:maps1152:MAPS_1152_sm_online-supplemental-plagioclase"></mediaResource><caption>Supporting info item</caption></supportingInfoItem><supportingInfoItem><mediaResource alt="supporting info item" href="urn-x:wiley:10869379:media:maps1152:MAPS_1152_sm_online-supplemental-pyroxene"></mediaResource><caption>Supporting info item</caption></supportingInfoItem></supportingInformation><abstractGroup><abstract type="main" xml:lang="en"><title type="main">Abstract–</title><p>Knowledge of Martian igneous basaltic compositions is crucial for constraining mantle evolution, including early differentiation and mantle convection. Primitive magmas provide direct information about their mantle source regions, but most Martian meteorites either contain cumulate olivine or crystallized from fractionated melts. The recently discovered Martian meteorite Northwest Africa (NWA) 5789 is an olivine‐phyric shergottite. NWA 5789 has special significance among the Martian meteorites because it appears to represent one of the most magnesian Martian magmas known, other than Yamato (Y) 980459. Its most magnesian olivine cores (Fo<sub>85</sub>) are in Mg‐Fe equilibrium with a magma of the bulk rock composition, suggesting that the bulk represents a magma composition. Based on the Al/Ti ratio of its pyroxenes, we infer that the rock began to crystallize at a high pressure consistent with conditions in Mars’ lower crust/upper mantle. It continued and completed its crystallization closer to the surface, where cooling was rapid and produced a mesostasis of radiating sprays of plagioclase and pyroxene. The mineralogy, petrology, mineral chemistry, and bulk rock composition of NWA 5789 are very similar to those of Y‐980459. The similarities between the two meteorites suggest that NWA 5789 (like Y‐980459) represents a primitive, mantle‐derived magma composition. They also suggest the possibility that NWA 5789 and Y‐980459 formed in the same lava flow. However, based on the mineralogy and texture of its mesostasis, NWA 5789 must have cooled more slowly than Y‐980459. NWA 5789 will help elucidate the igneous geology and geochemistry of Mars.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>Primitive olivine‐phyric shergottite NWA 5789: Petrography, mineral chemistry, and cooling history imply a magma similar to Yamato‐980459</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>Primitive olivine‐phyric shergottite NWA 5789</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>Primitive olivine‐phyric shergottite NWA 5789: Petrography, mineral chemistry, and cooling history imply a magma similar to Yamato‐980459</title></titleInfo><name type="personal"><namePart type="given">Juliane</namePart><namePart type="family">GROSS</namePart><affiliation>Lunar and Planetary Institute, 3600 Bay Area Boulevard, Houston, Texas 77058, USA</affiliation><description>Correspondence: Corresponding author. E‐mail: </description><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Allan H.</namePart><namePart type="family">TREIMAN</namePart><affiliation>Lunar and Planetary Institute, 3600 Bay Area Boulevard, Houston, Texas 77058, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Justin</namePart><namePart type="family">FILIBERTO</namePart><affiliation>Department of Earth Science MS‐126, Rice University, 6100 Main St., Houston, Texas 77005, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Christopher D. K.</namePart><namePart type="family">HERD</namePart><affiliation>Department of Earth and Atmospheric Sciences, University of Alberta, Edmonton, Alberta T6G 2E3, Canada</affiliation><role><roleTerm type="text">author</roleTerm></role></name><typeOfResource>text</typeOfResource><genre type="article" displayLabel="article"></genre><originInfo><publisher>Blackwell Publishing Ltd</publisher><place><placeTerm type="text">Oxford, UK</placeTerm></place><dateIssued encoding="w3cdtf">2011-01</dateIssued><edition>(Received 28 April 2010; revision accepted 30 September 2010)</edition><copyrightDate encoding="w3cdtf">2011</copyrightDate></originInfo><language><languageTerm type="code" authority="rfc3066">en</languageTerm><languageTerm type="code" authority="iso639-2b">eng</languageTerm></language><physicalDescription><internetMediaType>text/html</internetMediaType><extent unit="figures">13</extent><extent unit="tables">6</extent></physicalDescription><abstract lang="en">Knowledge of Martian igneous basaltic compositions is crucial for constraining mantle evolution, including early differentiation and mantle convection. Primitive magmas provide direct information about their mantle source regions, but most Martian meteorites either contain cumulate olivine or crystallized from fractionated melts. The recently discovered Martian meteorite Northwest Africa (NWA) 5789 is an olivine‐phyric shergottite. NWA 5789 has special significance among the Martian meteorites because it appears to represent one of the most magnesian Martian magmas known, other than Yamato (Y) 980459. Its most magnesian olivine cores (Fo85) are in Mg‐Fe equilibrium with a magma of the bulk rock composition, suggesting that the bulk represents a magma composition. Based on the Al/Ti ratio of its pyroxenes, we infer that the rock began to crystallize at a high pressure consistent with conditions in Mars’ lower crust/upper mantle. It continued and completed its crystallization closer to the surface, where cooling was rapid and produced a mesostasis of radiating sprays of plagioclase and pyroxene. The mineralogy, petrology, mineral chemistry, and bulk rock composition of NWA 5789 are very similar to those of Y‐980459. The similarities between the two meteorites suggest that NWA 5789 (like Y‐980459) represents a primitive, mantle‐derived magma composition. They also suggest the possibility that NWA 5789 and Y‐980459 formed in the same lava flow. However, based on the mineralogy and texture of its mesostasis, NWA 5789 must have cooled more slowly than Y‐980459. NWA 5789 will help elucidate the igneous geology and geochemistry of Mars.</abstract><relatedItem type="host"><titleInfo><title>Meteoritics & Planetary Science</title></titleInfo><genre type="journal">journal</genre><note type="content"> Table S1. Microprobe analyses of olivine. Table S2. Microprobe analyses of pyroxene. Table S3. Microprobe analyses of plagioclase. Table S1. Microprobe analyses of olivine. Table S2. Microprobe analyses of pyroxene. Table S3. Microprobe analyses of plagioclase. Table S1. Microprobe analyses of olivine. Table S2. Microprobe analyses of pyroxene. Table S3. Microprobe analyses of plagioclase.Supporting Info Item: Supporting info item - Supporting info item - Supporting info item - </note><identifier type="ISSN">1086-9379</identifier><identifier type="eISSN">1945-5100</identifier><identifier type="DOI">10.1111/(ISSN)1945-5100</identifier><identifier type="PublisherID">MAPS</identifier><part><date>2011</date><detail type="volume"><caption>vol.</caption><number>46</number></detail><detail type="issue"><caption>no.</caption><number>1</number></detail><extent unit="pages"><start>116</start><end>133</end><total>18</total></extent></part></relatedItem><identifier type="istex">0DE34CF31ED2C8BBEA689BE3AC0D74FFC6A96C78</identifier><identifier type="DOI">10.1111/j.1945-5100.2010.01152.x</identifier><identifier type="ArticleID">MAPS1152</identifier><accessCondition type="use and reproduction" contentType="copyright">© The Meteoritical Society, 2011</accessCondition><recordInfo><recordContentSource>WILEY</recordContentSource><recordOrigin>Blackwell Publishing Ltd</recordOrigin></recordInfo></mods></metadata><serie></serie></istex></record>Pour manipuler ce document sous Unix (Dilib)
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