Characterization and petrologic interpretation of olivine-rich basalts at Gusev Crater, Mars
Rocks on the floor of Gusev crater are basalts of uniform composition and mineralogy. Olivine, the only mineral to have been identified or inferred from data by all instruments on the Spirit rover, is especially abundant in these rocks. These picritic basalts are similar in many respects to certain...
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| creator | McSween, H. Y. Wyatt, M. B Gellert, R. Bell III, J. F. Morris, R. V. Herkenhoff, K. E. Crumpler, L. S. Milam, K. A. Stockstill, K. R. Tornabene, L. L. Arvidson, R. E. Bartlett, P. Blaney, D. Cabrol, N. A. Christensen, P. R. Clark, B. C. Crisp, J. A. Des Marais, D. J. Economou, T. Farmer, J. D. Farrand, W. Ghosh, A. Golombek, M. Gorevan, S. Greeley, R. Hamilton, V. E. Johnson, J. R. Joliff, B. L. Klingelhöfer, G. Knudson, A. T. McLennan, S. Ming, D. Moersch, J. E. Rieder, R. Ruff, S. W. Schröder, C. de Souza Jr, P. A. Squyres, S. W. Wänke, H. Wang, A. Yen, A. Zipfel, J. |
| description | Rocks on the floor of Gusev crater are basalts of uniform composition and mineralogy. Olivine, the only mineral to have been identified or inferred from data by all instruments on the Spirit rover, is especially abundant in these rocks. These picritic basalts are similar in many respects to certain Martian meteorites (olivine‐phyric shergottites). The olivine megacrysts in both have intermediate compositions, with modal abundances ranging up to 20–30%. Associated minerals in both include low‐calcium and high‐calcium pyroxenes, plagioclase of intermediate composition, iron‐titanium‐chromium oxides, and phosphate. These rocks also share minor element trends, reflected in their nickel‐magnesium and chromium‐magnesium ratios. Gusev basalts and shergottites appear to have formed from primitive magmas produced by melting an undepleted mantle at depth and erupted without significant fractionation. However, apparent differences between Gusev rocks and shergottites in their ages, plagioclase abundances, and volatile contents preclude direct correlation. Orbital determinations of global olivine distribution and compositions by thermal emission spectroscopy suggest that olivine‐rich rocks may be widespread. Because weathering under acidic conditions preferentially attacks olivine and disguises such rocks beneath alteration rinds, picritic basalts formed from primitive magmas may even be a common component of the Martian crust formed during ancient and recent times. |
| doi_str_mv | 10.1029/2005JE002477 |
| format | Article |
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Y. ; Wyatt, M. B ; Gellert, R. ; Bell III, J. F. ; Morris, R. V. ; Herkenhoff, K. E. ; Crumpler, L. S. ; Milam, K. A. ; Stockstill, K. R. ; Tornabene, L. L. ; Arvidson, R. E. ; Bartlett, P. ; Blaney, D. ; Cabrol, N. A. ; Christensen, P. R. ; Clark, B. C. ; Crisp, J. A. ; Des Marais, D. J. ; Economou, T. ; Farmer, J. D. ; Farrand, W. ; Ghosh, A. ; Golombek, M. ; Gorevan, S. ; Greeley, R. ; Hamilton, V. E. ; Johnson, J. R. ; Joliff, B. L. ; Klingelhöfer, G. ; Knudson, A. T. ; McLennan, S. ; Ming, D. ; Moersch, J. E. ; Rieder, R. ; Ruff, S. W. ; Schröder, C. ; de Souza Jr, P. A. ; Squyres, S. W. ; Wänke, H. ; Wang, A. ; Yen, A. ; Zipfel, J.</creator><creatorcontrib>McSween, H. Y. ; Wyatt, M. B ; Gellert, R. ; Bell III, J. F. ; Morris, R. V. ; Herkenhoff, K. E. ; Crumpler, L. S. ; Milam, K. A. ; Stockstill, K. R. ; Tornabene, L. L. ; Arvidson, R. E. ; Bartlett, P. ; Blaney, D. ; Cabrol, N. A. ; Christensen, P. R. ; Clark, B. C. ; Crisp, J. A. ; Des Marais, D. J. ; Economou, T. ; Farmer, J. D. ; Farrand, W. ; Ghosh, A. ; Golombek, M. ; Gorevan, S. ; Greeley, R. ; Hamilton, V. E. ; Johnson, J. R. ; Joliff, B. L. ; Klingelhöfer, G. ; Knudson, A. T. ; McLennan, S. ; Ming, D. ; Moersch, J. E. ; Rieder, R. ; Ruff, S. W. ; Schröder, C. ; de Souza Jr, P. A. ; Squyres, S. W. ; Wänke, H. ; Wang, A. ; Yen, A. ; Zipfel, J.</creatorcontrib><description>Rocks on the floor of Gusev crater are basalts of uniform composition and mineralogy. Olivine, the only mineral to have been identified or inferred from data by all instruments on the Spirit rover, is especially abundant in these rocks. These picritic basalts are similar in many respects to certain Martian meteorites (olivine‐phyric shergottites). The olivine megacrysts in both have intermediate compositions, with modal abundances ranging up to 20–30%. Associated minerals in both include low‐calcium and high‐calcium pyroxenes, plagioclase of intermediate composition, iron‐titanium‐chromium oxides, and phosphate. These rocks also share minor element trends, reflected in their nickel‐magnesium and chromium‐magnesium ratios. Gusev basalts and shergottites appear to have formed from primitive magmas produced by melting an undepleted mantle at depth and erupted without significant fractionation. However, apparent differences between Gusev rocks and shergottites in their ages, plagioclase abundances, and volatile contents preclude direct correlation. Orbital determinations of global olivine distribution and compositions by thermal emission spectroscopy suggest that olivine‐rich rocks may be widespread. Because weathering under acidic conditions preferentially attacks olivine and disguises such rocks beneath alteration rinds, picritic basalts formed from primitive magmas may even be a common component of the Martian crust formed during ancient and recent times.</description><identifier>ISSN: 0148-0227</identifier><identifier>ISSN: 2169-9097</identifier><identifier>EISSN: 2156-2202</identifier><identifier>EISSN: 2169-9100</identifier><identifier>DOI: 10.1029/2005JE002477</identifier><language>eng</language><publisher>Blackwell Publishing Ltd</publisher><subject>Basalt ; Craters ; Magma ; Mars ; Martian meteorites ; Minerals ; Olivine ; Plagioclase ; Rocks ; Shergottites</subject><ispartof>Journal of Geophysical Research. E. Planets, 2006-01, Vol.111 (E2), p.n/a</ispartof><rights>Copyright 2006 by the American Geophysical Union.</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-a5695-2093787b560dfd700562be02dcb71e1fcf009d60a833dc6943be67d633768f153</citedby><cites>FETCH-LOGICAL-a5695-2093787b560dfd700562be02dcb71e1fcf009d60a833dc6943be67d633768f153</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://onlinelibrary.wiley.com/doi/pdf/10.1029%2F2005JE002477$$EPDF$$P50$$Gwiley$$H</linktopdf><linktohtml>$$Uhttps://onlinelibrary.wiley.com/doi/full/10.1029%2F2005JE002477$$EHTML$$P50$$Gwiley$$H</linktohtml><link.rule.ids>314,780,784,1417,1433,11514,27924,27925,45574,45575,46409,46468,46833,46892</link.rule.ids></links><search><creatorcontrib>McSween, H. Y.</creatorcontrib><creatorcontrib>Wyatt, M. B</creatorcontrib><creatorcontrib>Gellert, R.</creatorcontrib><creatorcontrib>Bell III, J. F.</creatorcontrib><creatorcontrib>Morris, R. V.</creatorcontrib><creatorcontrib>Herkenhoff, K. E.</creatorcontrib><creatorcontrib>Crumpler, L. S.</creatorcontrib><creatorcontrib>Milam, K. A.</creatorcontrib><creatorcontrib>Stockstill, K. R.</creatorcontrib><creatorcontrib>Tornabene, L. L.</creatorcontrib><creatorcontrib>Arvidson, R. E.</creatorcontrib><creatorcontrib>Bartlett, P.</creatorcontrib><creatorcontrib>Blaney, D.</creatorcontrib><creatorcontrib>Cabrol, N. A.</creatorcontrib><creatorcontrib>Christensen, P. R.</creatorcontrib><creatorcontrib>Clark, B. C.</creatorcontrib><creatorcontrib>Crisp, J. A.</creatorcontrib><creatorcontrib>Des Marais, D. J.</creatorcontrib><creatorcontrib>Economou, T.</creatorcontrib><creatorcontrib>Farmer, J. D.</creatorcontrib><creatorcontrib>Farrand, W.</creatorcontrib><creatorcontrib>Ghosh, A.</creatorcontrib><creatorcontrib>Golombek, M.</creatorcontrib><creatorcontrib>Gorevan, S.</creatorcontrib><creatorcontrib>Greeley, R.</creatorcontrib><creatorcontrib>Hamilton, V. E.</creatorcontrib><creatorcontrib>Johnson, J. R.</creatorcontrib><creatorcontrib>Joliff, B. L.</creatorcontrib><creatorcontrib>Klingelhöfer, G.</creatorcontrib><creatorcontrib>Knudson, A. T.</creatorcontrib><creatorcontrib>McLennan, S.</creatorcontrib><creatorcontrib>Ming, D.</creatorcontrib><creatorcontrib>Moersch, J. E.</creatorcontrib><creatorcontrib>Rieder, R.</creatorcontrib><creatorcontrib>Ruff, S. W.</creatorcontrib><creatorcontrib>Schröder, C.</creatorcontrib><creatorcontrib>de Souza Jr, P. A.</creatorcontrib><creatorcontrib>Squyres, S. W.</creatorcontrib><creatorcontrib>Wänke, H.</creatorcontrib><creatorcontrib>Wang, A.</creatorcontrib><creatorcontrib>Yen, A.</creatorcontrib><creatorcontrib>Zipfel, J.</creatorcontrib><title>Characterization and petrologic interpretation of olivine-rich basalts at Gusev Crater, Mars</title><title>Journal of Geophysical Research. E. Planets</title><addtitle>J. Geophys. Res</addtitle><description>Rocks on the floor of Gusev crater are basalts of uniform composition and mineralogy. Olivine, the only mineral to have been identified or inferred from data by all instruments on the Spirit rover, is especially abundant in these rocks. These picritic basalts are similar in many respects to certain Martian meteorites (olivine‐phyric shergottites). The olivine megacrysts in both have intermediate compositions, with modal abundances ranging up to 20–30%. Associated minerals in both include low‐calcium and high‐calcium pyroxenes, plagioclase of intermediate composition, iron‐titanium‐chromium oxides, and phosphate. These rocks also share minor element trends, reflected in their nickel‐magnesium and chromium‐magnesium ratios. Gusev basalts and shergottites appear to have formed from primitive magmas produced by melting an undepleted mantle at depth and erupted without significant fractionation. However, apparent differences between Gusev rocks and shergottites in their ages, plagioclase abundances, and volatile contents preclude direct correlation. Orbital determinations of global olivine distribution and compositions by thermal emission spectroscopy suggest that olivine‐rich rocks may be widespread. Because weathering under acidic conditions preferentially attacks olivine and disguises such rocks beneath alteration rinds, picritic basalts formed from primitive magmas may even be a common component of the Martian crust formed during ancient and recent times.</description><subject>Basalt</subject><subject>Craters</subject><subject>Magma</subject><subject>Mars</subject><subject>Martian meteorites</subject><subject>Minerals</subject><subject>Olivine</subject><subject>Plagioclase</subject><subject>Rocks</subject><subject>Shergottites</subject><issn>0148-0227</issn><issn>2169-9097</issn><issn>2156-2202</issn><issn>2169-9100</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2006</creationdate><recordtype>article</recordtype><recordid>eNqFkUtP3TAQha2qSL0CdvwAryoWpIzH8WvZ3t6GZyshUDeVLCdximlILnYur19PIKhixZ3NLM53jjRzCNlh8IUBmn0EEEcLAMyV-kBmyITMEAE_khmwXGeAqD6R7ZSuYJxcyBzYjPyZX7roqsHH8OiG0HfUdTVd-iH2bf83VDR0o7aMfpjUvqF9G25D57MYqktauuTaIVE30GKV_C2dRzca9uipi2mLbDSuTX77dW-Six-L8_lBdvKrOJx_PcmckEZkCIYrrUohoW5qNd4hsfSAdVUq5llTNQCmluA053UlTc5LL1UtOVdSN0zwTfJ5yl3G_mbl02CvQ6p827rO96tkUTPkmuXrQWU0R5RrQaZyzbh4TtxdA3IAzZhWI7o3oVXsU4q-scsYrl18sAzsc4X2bYUjjhN-F1r_8C5rj4qzBcLLJ7LJFNLg7_-bXPxnpeJK2N8_C2uOzXdTHHyzmj8BI32qCQ</recordid><startdate>20060101</startdate><enddate>20060101</enddate><creator>McSween, H. 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L. ; Arvidson, R. E. ; Bartlett, P. ; Blaney, D. ; Cabrol, N. A. ; Christensen, P. R. ; Clark, B. C. ; Crisp, J. A. ; Des Marais, D. J. ; Economou, T. ; Farmer, J. D. ; Farrand, W. ; Ghosh, A. ; Golombek, M. ; Gorevan, S. ; Greeley, R. ; Hamilton, V. E. ; Johnson, J. R. ; Joliff, B. L. ; Klingelhöfer, G. ; Knudson, A. T. ; McLennan, S. ; Ming, D. ; Moersch, J. E. ; Rieder, R. ; Ruff, S. W. ; Schröder, C. ; de Souza Jr, P. A. ; Squyres, S. W. ; Wänke, H. ; Wang, A. ; Yen, A. ; Zipfel, J.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a5695-2093787b560dfd700562be02dcb71e1fcf009d60a833dc6943be67d633768f153</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2006</creationdate><topic>Basalt</topic><topic>Craters</topic><topic>Magma</topic><topic>Mars</topic><topic>Martian meteorites</topic><topic>Minerals</topic><topic>Olivine</topic><topic>Plagioclase</topic><topic>Rocks</topic><topic>Shergottites</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>McSween, H. Y.</creatorcontrib><creatorcontrib>Wyatt, M. B</creatorcontrib><creatorcontrib>Gellert, R.</creatorcontrib><creatorcontrib>Bell III, J. F.</creatorcontrib><creatorcontrib>Morris, R. V.</creatorcontrib><creatorcontrib>Herkenhoff, K. E.</creatorcontrib><creatorcontrib>Crumpler, L. S.</creatorcontrib><creatorcontrib>Milam, K. 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W.</creatorcontrib><creatorcontrib>Wänke, H.</creatorcontrib><creatorcontrib>Wang, A.</creatorcontrib><creatorcontrib>Yen, A.</creatorcontrib><creatorcontrib>Zipfel, J.</creatorcontrib><collection>Istex</collection><collection>CrossRef</collection><collection>Aluminium Industry Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Materials Research Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Solid State and Superconductivity Abstracts</collection><collection>Engineering Research Database</collection><collection>Civil Engineering Abstracts</collection><jtitle>Journal of Geophysical Research. E. Planets</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>McSween, H. Y.</au><au>Wyatt, M. B</au><au>Gellert, R.</au><au>Bell III, J. F.</au><au>Morris, R. V.</au><au>Herkenhoff, K. E.</au><au>Crumpler, L. S.</au><au>Milam, K. A.</au><au>Stockstill, K. R.</au><au>Tornabene, L. L.</au><au>Arvidson, R. E.</au><au>Bartlett, P.</au><au>Blaney, D.</au><au>Cabrol, N. A.</au><au>Christensen, P. R.</au><au>Clark, B. C.</au><au>Crisp, J. A.</au><au>Des Marais, D. J.</au><au>Economou, T.</au><au>Farmer, J. D.</au><au>Farrand, W.</au><au>Ghosh, A.</au><au>Golombek, M.</au><au>Gorevan, S.</au><au>Greeley, R.</au><au>Hamilton, V. E.</au><au>Johnson, J. R.</au><au>Joliff, B. L.</au><au>Klingelhöfer, G.</au><au>Knudson, A. T.</au><au>McLennan, S.</au><au>Ming, D.</au><au>Moersch, J. E.</au><au>Rieder, R.</au><au>Ruff, S. W.</au><au>Schröder, C.</au><au>de Souza Jr, P. A.</au><au>Squyres, S. W.</au><au>Wänke, H.</au><au>Wang, A.</au><au>Yen, A.</au><au>Zipfel, J.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Characterization and petrologic interpretation of olivine-rich basalts at Gusev Crater, Mars</atitle><jtitle>Journal of Geophysical Research. E. Planets</jtitle><addtitle>J. Geophys. Res</addtitle><date>2006-01-01</date><risdate>2006</risdate><volume>111</volume><issue>E2</issue><epage>n/a</epage><issn>0148-0227</issn><issn>2169-9097</issn><eissn>2156-2202</eissn><eissn>2169-9100</eissn><abstract>Rocks on the floor of Gusev crater are basalts of uniform composition and mineralogy. Olivine, the only mineral to have been identified or inferred from data by all instruments on the Spirit rover, is especially abundant in these rocks. These picritic basalts are similar in many respects to certain Martian meteorites (olivine‐phyric shergottites). The olivine megacrysts in both have intermediate compositions, with modal abundances ranging up to 20–30%. Associated minerals in both include low‐calcium and high‐calcium pyroxenes, plagioclase of intermediate composition, iron‐titanium‐chromium oxides, and phosphate. These rocks also share minor element trends, reflected in their nickel‐magnesium and chromium‐magnesium ratios. Gusev basalts and shergottites appear to have formed from primitive magmas produced by melting an undepleted mantle at depth and erupted without significant fractionation. However, apparent differences between Gusev rocks and shergottites in their ages, plagioclase abundances, and volatile contents preclude direct correlation. Orbital determinations of global olivine distribution and compositions by thermal emission spectroscopy suggest that olivine‐rich rocks may be widespread. Because weathering under acidic conditions preferentially attacks olivine and disguises such rocks beneath alteration rinds, picritic basalts formed from primitive magmas may even be a common component of the Martian crust formed during ancient and recent times.</abstract><pub>Blackwell Publishing Ltd</pub><doi>10.1029/2005JE002477</doi><tpages>17</tpages><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0148-0227 |
| ispartof | Journal of Geophysical Research. E. Planets, 2006-01, Vol.111 (E2), p.n/a |
| issn | 0148-0227 2169-9097 2156-2202 2169-9100 |
| language | eng |
| recordid | cdi_proquest_miscellaneous_28123814 |
| source | Access via Wiley Online Library; Wiley Free Content; Wiley-Blackwell AGU Digital Library; Alma/SFX Local Collection |
| subjects | Basalt Craters Magma Mars Martian meteorites Minerals Olivine Plagioclase Rocks Shergottites |
| title | Characterization and petrologic interpretation of olivine-rich basalts at Gusev Crater, Mars |
| url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2024-12-18T23%3A02%3A14IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_cross&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=Characterization%20and%20petrologic%20interpretation%20of%20olivine-rich%20basalts%20at%20Gusev%20Crater,%20Mars&rft.jtitle=Journal%20of%20Geophysical%20Research.%20E.%20Planets&rft.au=McSween,%20H.%20Y.&rft.date=2006-01-01&rft.volume=111&rft.issue=E2&rft.epage=n/a&rft.issn=0148-0227&rft.eissn=2156-2202&rft_id=info:doi/10.1029/2005JE002477&rft_dat=%3Cproquest_cross%3E17481354%3C/proquest_cross%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_pqid=1730081187&rft_id=info:pmid/&rfr_iscdi=true |