Modal abundances of pyroxene, olivine, and mesostasis in nakhlites: Heterogeneity, variation, and implications for nakhlite emplacement
Nakhlites, clinopyroxenite meteorites from Mars, share common crystallization and ejection ages, suggesting that they might have been ejected from the same place on Mars by the same ejection event (impact) and are different samples of the same thick volcanic flow unit or shallow sill. Mean modal abu...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Corrigan, Catherine M [verfasserIn] |
|---|
| Format: |
Artikel |
|---|---|
| Sprache: |
Englisch |
| Erschienen: |
2015 |
|---|
| Rechteinformationen: |
Nutzungsrecht: © Published 2015. This article is a U.S. Government work and is in the public domain in the USA. © COPYRIGHT 2015 Wiley Subscription Services, Inc. |
|---|
| Schlagwörter: |
|---|
| Übergeordnetes Werk: |
Enthalten in: Meteoritics & planetary science - Lawrence, Kan. : Allen Press, 1996, 50(2015), 9, Seite 1497-1511 |
|---|---|
| Übergeordnetes Werk: |
volume:50 ; year:2015 ; number:9 ; pages:1497-1511 |
| Links: |
|---|
| DOI / URN: |
10.1111/maps.12492 |
|---|
| Katalog-ID: |
OLC1965317952 |
|---|
| LEADER | 01000caa a2200265 4500 | ||
|---|---|---|---|
| 001 | OLC1965317952 | ||
| 003 | DE-627 | ||
| 005 | 20230714163708.0 | ||
| 007 | tu | ||
| 008 | 160206s2015 xx ||||| 00| ||eng c | ||
| 024 | 7 | |a 10.1111/maps.12492 |2 doi | |
| 028 | 5 | 2 | |a PQ20160617 |
| 035 | |a (DE-627)OLC1965317952 | ||
| 035 | |a (DE-599)GBVOLC1965317952 | ||
| 035 | |a (PRQ)c2402-94fb005993b5c1f676bc96b5853876519a8f653ce2ecf2a7149c1c644ce676300 | ||
| 035 | |a (KEY)0042930920150000050000901497modalabundancesofpyroxeneolivineandmesostasisinnak | ||
| 040 | |a DE-627 |b ger |c DE-627 |e rakwb | ||
| 041 | |a eng | ||
| 082 | 0 | 4 | |a 520 |a 550 |q DNB |
| 100 | 1 | |a Corrigan, Catherine M |e verfasserin |4 aut | |
| 245 | 1 | 0 | |a Modal abundances of pyroxene, olivine, and mesostasis in nakhlites: Heterogeneity, variation, and implications for nakhlite emplacement |
| 264 | 1 | |c 2015 | |
| 336 | |a Text |b txt |2 rdacontent | ||
| 337 | |a ohne Hilfsmittel zu benutzen |b n |2 rdamedia | ||
| 338 | |a Band |b nc |2 rdacarrier | ||
| 520 | |a Nakhlites, clinopyroxenite meteorites from Mars, share common crystallization and ejection ages, suggesting that they might have been ejected from the same place on Mars by the same ejection event (impact) and are different samples of the same thick volcanic flow unit or shallow sill. Mean modal abundances and abundance ranges of pyroxene, olivine, and mesostasis vary widely among different thin‐sections of an individual nakhlite. Lithologic heterogeneity is the main factor contributing to the observed modal‐abundance variations measured in thin‐sections prepared from different fragments of the same stone. Two groups of nakhlites are distinguished from one another by which major constituent varies the least and the abundance of that constituent. The group consisting of Nakhla, Lafayette, Governador Valadares, and the Yamato nakhlite pairing group is characterized by low modal mesostasis and pyroxene‐olivine covariance, whereas the group consisting of the Miller Range nakhlite pairing group and Northwest Africa 5790 is characterized by low modal olivine and pyroxene‐mesostasis covariance. These two groups sample the slowest‐cooled interior portion and the chilled margin, respectively, of the nakhlite emplacement body as presently understood, and appear to be also related to recently proposed nakhlite groups independently established using compositional rather than petrographic observations. Phenocryst modal abundances vary with inferred depth in the nakhlite igneous body in a manner consistent with solidification of the nakhlite stack from dynamically sorted phenocryst‐rich magmatic crystal‐liquid mush. | ||
| 540 | |a Nutzungsrecht: © Published 2015. This article is a U.S. Government work and is in the public domain in the USA. | ||
| 540 | |a © COPYRIGHT 2015 Wiley Subscription Services, Inc. | ||
| 650 | 4 | |a Meteorites | |
| 650 | 4 | |a Pyroxene | |
| 650 | 4 | |a Magma | |
| 700 | 1 | |a Velbel, Michael A |4 oth | |
| 700 | 1 | |a Vicenzi, Edward P |4 oth | |
| 773 | 0 | 8 | |i Enthalten in |t Meteoritics & planetary science |d Lawrence, Kan. : Allen Press, 1996 |g 50(2015), 9, Seite 1497-1511 |w (DE-627)193298368 |w (DE-600)1306943-3 |w (DE-576)060237333 |x 1086-9379 |7 nnns |
| 773 | 1 | 8 | |g volume:50 |g year:2015 |g number:9 |g pages:1497-1511 |
| 856 | 4 | 1 | |u http://dx.doi.org/10.1111/maps.12492 |3 Volltext |
| 856 | 4 | 2 | |u http://onlinelibrary.wiley.com/doi/10.1111/maps.12492/abstract |
| 856 | 4 | 2 | |u http://search.proquest.com/docview/1709479309 |
| 912 | |a GBV_USEFLAG_A | ||
| 912 | |a SYSFLAG_A | ||
| 912 | |a GBV_OLC | ||
| 912 | |a SSG-OLC-GEO | ||
| 912 | |a SSG-OLC-AST | ||
| 912 | |a SSG-OPC-GGO | ||
| 912 | |a SSG-OPC-AST | ||
| 912 | |a GBV_ILN_2004 | ||
| 951 | |a AR | ||
| 952 | |d 50 |j 2015 |e 9 |h 1497-1511 | ||
| author_variant |
c m c cm cmc |
|---|---|
| matchkey_str |
article:10869379:2015----::oaaudneoprxnoiienmssaiinkltseeoeetvrainnip |
| hierarchy_sort_str |
2015 |
| publishDate |
2015 |
| allfields |
10.1111/maps.12492 doi PQ20160617 (DE-627)OLC1965317952 (DE-599)GBVOLC1965317952 (PRQ)c2402-94fb005993b5c1f676bc96b5853876519a8f653ce2ecf2a7149c1c644ce676300 (KEY)0042930920150000050000901497modalabundancesofpyroxeneolivineandmesostasisinnak DE-627 ger DE-627 rakwb eng 520 550 DNB Corrigan, Catherine M verfasserin aut Modal abundances of pyroxene, olivine, and mesostasis in nakhlites: Heterogeneity, variation, and implications for nakhlite emplacement 2015 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Nakhlites, clinopyroxenite meteorites from Mars, share common crystallization and ejection ages, suggesting that they might have been ejected from the same place on Mars by the same ejection event (impact) and are different samples of the same thick volcanic flow unit or shallow sill. Mean modal abundances and abundance ranges of pyroxene, olivine, and mesostasis vary widely among different thin‐sections of an individual nakhlite. Lithologic heterogeneity is the main factor contributing to the observed modal‐abundance variations measured in thin‐sections prepared from different fragments of the same stone. Two groups of nakhlites are distinguished from one another by which major constituent varies the least and the abundance of that constituent. The group consisting of Nakhla, Lafayette, Governador Valadares, and the Yamato nakhlite pairing group is characterized by low modal mesostasis and pyroxene‐olivine covariance, whereas the group consisting of the Miller Range nakhlite pairing group and Northwest Africa 5790 is characterized by low modal olivine and pyroxene‐mesostasis covariance. These two groups sample the slowest‐cooled interior portion and the chilled margin, respectively, of the nakhlite emplacement body as presently understood, and appear to be also related to recently proposed nakhlite groups independently established using compositional rather than petrographic observations. Phenocryst modal abundances vary with inferred depth in the nakhlite igneous body in a manner consistent with solidification of the nakhlite stack from dynamically sorted phenocryst‐rich magmatic crystal‐liquid mush. Nutzungsrecht: © Published 2015. This article is a U.S. Government work and is in the public domain in the USA. © COPYRIGHT 2015 Wiley Subscription Services, Inc. Meteorites Pyroxene Magma Velbel, Michael A oth Vicenzi, Edward P oth Enthalten in Meteoritics & planetary science Lawrence, Kan. : Allen Press, 1996 50(2015), 9, Seite 1497-1511 (DE-627)193298368 (DE-600)1306943-3 (DE-576)060237333 1086-9379 nnns volume:50 year:2015 number:9 pages:1497-1511 http://dx.doi.org/10.1111/maps.12492 Volltext http://onlinelibrary.wiley.com/doi/10.1111/maps.12492/abstract http://search.proquest.com/docview/1709479309 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-GEO SSG-OLC-AST SSG-OPC-GGO SSG-OPC-AST GBV_ILN_2004 AR 50 2015 9 1497-1511 |
| spelling |
10.1111/maps.12492 doi PQ20160617 (DE-627)OLC1965317952 (DE-599)GBVOLC1965317952 (PRQ)c2402-94fb005993b5c1f676bc96b5853876519a8f653ce2ecf2a7149c1c644ce676300 (KEY)0042930920150000050000901497modalabundancesofpyroxeneolivineandmesostasisinnak DE-627 ger DE-627 rakwb eng 520 550 DNB Corrigan, Catherine M verfasserin aut Modal abundances of pyroxene, olivine, and mesostasis in nakhlites: Heterogeneity, variation, and implications for nakhlite emplacement 2015 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Nakhlites, clinopyroxenite meteorites from Mars, share common crystallization and ejection ages, suggesting that they might have been ejected from the same place on Mars by the same ejection event (impact) and are different samples of the same thick volcanic flow unit or shallow sill. Mean modal abundances and abundance ranges of pyroxene, olivine, and mesostasis vary widely among different thin‐sections of an individual nakhlite. Lithologic heterogeneity is the main factor contributing to the observed modal‐abundance variations measured in thin‐sections prepared from different fragments of the same stone. Two groups of nakhlites are distinguished from one another by which major constituent varies the least and the abundance of that constituent. The group consisting of Nakhla, Lafayette, Governador Valadares, and the Yamato nakhlite pairing group is characterized by low modal mesostasis and pyroxene‐olivine covariance, whereas the group consisting of the Miller Range nakhlite pairing group and Northwest Africa 5790 is characterized by low modal olivine and pyroxene‐mesostasis covariance. These two groups sample the slowest‐cooled interior portion and the chilled margin, respectively, of the nakhlite emplacement body as presently understood, and appear to be also related to recently proposed nakhlite groups independently established using compositional rather than petrographic observations. Phenocryst modal abundances vary with inferred depth in the nakhlite igneous body in a manner consistent with solidification of the nakhlite stack from dynamically sorted phenocryst‐rich magmatic crystal‐liquid mush. Nutzungsrecht: © Published 2015. This article is a U.S. Government work and is in the public domain in the USA. © COPYRIGHT 2015 Wiley Subscription Services, Inc. Meteorites Pyroxene Magma Velbel, Michael A oth Vicenzi, Edward P oth Enthalten in Meteoritics & planetary science Lawrence, Kan. : Allen Press, 1996 50(2015), 9, Seite 1497-1511 (DE-627)193298368 (DE-600)1306943-3 (DE-576)060237333 1086-9379 nnns volume:50 year:2015 number:9 pages:1497-1511 http://dx.doi.org/10.1111/maps.12492 Volltext http://onlinelibrary.wiley.com/doi/10.1111/maps.12492/abstract http://search.proquest.com/docview/1709479309 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-GEO SSG-OLC-AST SSG-OPC-GGO SSG-OPC-AST GBV_ILN_2004 AR 50 2015 9 1497-1511 |
| allfields_unstemmed |
10.1111/maps.12492 doi PQ20160617 (DE-627)OLC1965317952 (DE-599)GBVOLC1965317952 (PRQ)c2402-94fb005993b5c1f676bc96b5853876519a8f653ce2ecf2a7149c1c644ce676300 (KEY)0042930920150000050000901497modalabundancesofpyroxeneolivineandmesostasisinnak DE-627 ger DE-627 rakwb eng 520 550 DNB Corrigan, Catherine M verfasserin aut Modal abundances of pyroxene, olivine, and mesostasis in nakhlites: Heterogeneity, variation, and implications for nakhlite emplacement 2015 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Nakhlites, clinopyroxenite meteorites from Mars, share common crystallization and ejection ages, suggesting that they might have been ejected from the same place on Mars by the same ejection event (impact) and are different samples of the same thick volcanic flow unit or shallow sill. Mean modal abundances and abundance ranges of pyroxene, olivine, and mesostasis vary widely among different thin‐sections of an individual nakhlite. Lithologic heterogeneity is the main factor contributing to the observed modal‐abundance variations measured in thin‐sections prepared from different fragments of the same stone. Two groups of nakhlites are distinguished from one another by which major constituent varies the least and the abundance of that constituent. The group consisting of Nakhla, Lafayette, Governador Valadares, and the Yamato nakhlite pairing group is characterized by low modal mesostasis and pyroxene‐olivine covariance, whereas the group consisting of the Miller Range nakhlite pairing group and Northwest Africa 5790 is characterized by low modal olivine and pyroxene‐mesostasis covariance. These two groups sample the slowest‐cooled interior portion and the chilled margin, respectively, of the nakhlite emplacement body as presently understood, and appear to be also related to recently proposed nakhlite groups independently established using compositional rather than petrographic observations. Phenocryst modal abundances vary with inferred depth in the nakhlite igneous body in a manner consistent with solidification of the nakhlite stack from dynamically sorted phenocryst‐rich magmatic crystal‐liquid mush. Nutzungsrecht: © Published 2015. This article is a U.S. Government work and is in the public domain in the USA. © COPYRIGHT 2015 Wiley Subscription Services, Inc. Meteorites Pyroxene Magma Velbel, Michael A oth Vicenzi, Edward P oth Enthalten in Meteoritics & planetary science Lawrence, Kan. : Allen Press, 1996 50(2015), 9, Seite 1497-1511 (DE-627)193298368 (DE-600)1306943-3 (DE-576)060237333 1086-9379 nnns volume:50 year:2015 number:9 pages:1497-1511 http://dx.doi.org/10.1111/maps.12492 Volltext http://onlinelibrary.wiley.com/doi/10.1111/maps.12492/abstract http://search.proquest.com/docview/1709479309 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-GEO SSG-OLC-AST SSG-OPC-GGO SSG-OPC-AST GBV_ILN_2004 AR 50 2015 9 1497-1511 |
| allfieldsGer |
10.1111/maps.12492 doi PQ20160617 (DE-627)OLC1965317952 (DE-599)GBVOLC1965317952 (PRQ)c2402-94fb005993b5c1f676bc96b5853876519a8f653ce2ecf2a7149c1c644ce676300 (KEY)0042930920150000050000901497modalabundancesofpyroxeneolivineandmesostasisinnak DE-627 ger DE-627 rakwb eng 520 550 DNB Corrigan, Catherine M verfasserin aut Modal abundances of pyroxene, olivine, and mesostasis in nakhlites: Heterogeneity, variation, and implications for nakhlite emplacement 2015 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Nakhlites, clinopyroxenite meteorites from Mars, share common crystallization and ejection ages, suggesting that they might have been ejected from the same place on Mars by the same ejection event (impact) and are different samples of the same thick volcanic flow unit or shallow sill. Mean modal abundances and abundance ranges of pyroxene, olivine, and mesostasis vary widely among different thin‐sections of an individual nakhlite. Lithologic heterogeneity is the main factor contributing to the observed modal‐abundance variations measured in thin‐sections prepared from different fragments of the same stone. Two groups of nakhlites are distinguished from one another by which major constituent varies the least and the abundance of that constituent. The group consisting of Nakhla, Lafayette, Governador Valadares, and the Yamato nakhlite pairing group is characterized by low modal mesostasis and pyroxene‐olivine covariance, whereas the group consisting of the Miller Range nakhlite pairing group and Northwest Africa 5790 is characterized by low modal olivine and pyroxene‐mesostasis covariance. These two groups sample the slowest‐cooled interior portion and the chilled margin, respectively, of the nakhlite emplacement body as presently understood, and appear to be also related to recently proposed nakhlite groups independently established using compositional rather than petrographic observations. Phenocryst modal abundances vary with inferred depth in the nakhlite igneous body in a manner consistent with solidification of the nakhlite stack from dynamically sorted phenocryst‐rich magmatic crystal‐liquid mush. Nutzungsrecht: © Published 2015. This article is a U.S. Government work and is in the public domain in the USA. © COPYRIGHT 2015 Wiley Subscription Services, Inc. Meteorites Pyroxene Magma Velbel, Michael A oth Vicenzi, Edward P oth Enthalten in Meteoritics & planetary science Lawrence, Kan. : Allen Press, 1996 50(2015), 9, Seite 1497-1511 (DE-627)193298368 (DE-600)1306943-3 (DE-576)060237333 1086-9379 nnns volume:50 year:2015 number:9 pages:1497-1511 http://dx.doi.org/10.1111/maps.12492 Volltext http://onlinelibrary.wiley.com/doi/10.1111/maps.12492/abstract http://search.proquest.com/docview/1709479309 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-GEO SSG-OLC-AST SSG-OPC-GGO SSG-OPC-AST GBV_ILN_2004 AR 50 2015 9 1497-1511 |
| allfieldsSound |
10.1111/maps.12492 doi PQ20160617 (DE-627)OLC1965317952 (DE-599)GBVOLC1965317952 (PRQ)c2402-94fb005993b5c1f676bc96b5853876519a8f653ce2ecf2a7149c1c644ce676300 (KEY)0042930920150000050000901497modalabundancesofpyroxeneolivineandmesostasisinnak DE-627 ger DE-627 rakwb eng 520 550 DNB Corrigan, Catherine M verfasserin aut Modal abundances of pyroxene, olivine, and mesostasis in nakhlites: Heterogeneity, variation, and implications for nakhlite emplacement 2015 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Nakhlites, clinopyroxenite meteorites from Mars, share common crystallization and ejection ages, suggesting that they might have been ejected from the same place on Mars by the same ejection event (impact) and are different samples of the same thick volcanic flow unit or shallow sill. Mean modal abundances and abundance ranges of pyroxene, olivine, and mesostasis vary widely among different thin‐sections of an individual nakhlite. Lithologic heterogeneity is the main factor contributing to the observed modal‐abundance variations measured in thin‐sections prepared from different fragments of the same stone. Two groups of nakhlites are distinguished from one another by which major constituent varies the least and the abundance of that constituent. The group consisting of Nakhla, Lafayette, Governador Valadares, and the Yamato nakhlite pairing group is characterized by low modal mesostasis and pyroxene‐olivine covariance, whereas the group consisting of the Miller Range nakhlite pairing group and Northwest Africa 5790 is characterized by low modal olivine and pyroxene‐mesostasis covariance. These two groups sample the slowest‐cooled interior portion and the chilled margin, respectively, of the nakhlite emplacement body as presently understood, and appear to be also related to recently proposed nakhlite groups independently established using compositional rather than petrographic observations. Phenocryst modal abundances vary with inferred depth in the nakhlite igneous body in a manner consistent with solidification of the nakhlite stack from dynamically sorted phenocryst‐rich magmatic crystal‐liquid mush. Nutzungsrecht: © Published 2015. This article is a U.S. Government work and is in the public domain in the USA. © COPYRIGHT 2015 Wiley Subscription Services, Inc. Meteorites Pyroxene Magma Velbel, Michael A oth Vicenzi, Edward P oth Enthalten in Meteoritics & planetary science Lawrence, Kan. : Allen Press, 1996 50(2015), 9, Seite 1497-1511 (DE-627)193298368 (DE-600)1306943-3 (DE-576)060237333 1086-9379 nnns volume:50 year:2015 number:9 pages:1497-1511 http://dx.doi.org/10.1111/maps.12492 Volltext http://onlinelibrary.wiley.com/doi/10.1111/maps.12492/abstract http://search.proquest.com/docview/1709479309 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-GEO SSG-OLC-AST SSG-OPC-GGO SSG-OPC-AST GBV_ILN_2004 AR 50 2015 9 1497-1511 |
| language |
English |
| source |
Enthalten in Meteoritics & planetary science 50(2015), 9, Seite 1497-1511 volume:50 year:2015 number:9 pages:1497-1511 |
| sourceStr |
Enthalten in Meteoritics & planetary science 50(2015), 9, Seite 1497-1511 volume:50 year:2015 number:9 pages:1497-1511 |
| format_phy_str_mv |
Article |
| institution |
findex.gbv.de |
| topic_facet |
Meteorites Pyroxene Magma |
| dewey-raw |
520 |
| isfreeaccess_bool |
false |
| container_title |
Meteoritics & planetary science |
| authorswithroles_txt_mv |
Corrigan, Catherine M @@aut@@ Velbel, Michael A @@oth@@ Vicenzi, Edward P @@oth@@ |
| publishDateDaySort_date |
2015-01-01T00:00:00Z |
| hierarchy_top_id |
193298368 |
| dewey-sort |
3520 |
| id |
OLC1965317952 |
| language_de |
englisch |
| fullrecord |
<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a2200265 4500</leader><controlfield tag="001">OLC1965317952</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20230714163708.0</controlfield><controlfield tag="007">tu</controlfield><controlfield tag="008">160206s2015 xx ||||| 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1111/maps.12492</subfield><subfield code="2">doi</subfield></datafield><datafield tag="028" ind1="5" ind2="2"><subfield code="a">PQ20160617</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)OLC1965317952</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-599)GBVOLC1965317952</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(PRQ)c2402-94fb005993b5c1f676bc96b5853876519a8f653ce2ecf2a7149c1c644ce676300</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(KEY)0042930920150000050000901497modalabundancesofpyroxeneolivineandmesostasisinnak</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-627</subfield><subfield code="b">ger</subfield><subfield code="c">DE-627</subfield><subfield code="e">rakwb</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="082" ind1="0" ind2="4"><subfield code="a">520</subfield><subfield code="a">550</subfield><subfield code="q">DNB</subfield></datafield><datafield tag="100" ind1="1" ind2=" "><subfield code="a">Corrigan, Catherine M</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Modal abundances of pyroxene, olivine, and mesostasis in nakhlites: Heterogeneity, variation, and implications for nakhlite emplacement</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2015</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">ohne Hilfsmittel zu benutzen</subfield><subfield code="b">n</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Band</subfield><subfield code="b">nc</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Nakhlites, clinopyroxenite meteorites from Mars, share common crystallization and ejection ages, suggesting that they might have been ejected from the same place on Mars by the same ejection event (impact) and are different samples of the same thick volcanic flow unit or shallow sill. Mean modal abundances and abundance ranges of pyroxene, olivine, and mesostasis vary widely among different thin‐sections of an individual nakhlite. Lithologic heterogeneity is the main factor contributing to the observed modal‐abundance variations measured in thin‐sections prepared from different fragments of the same stone. Two groups of nakhlites are distinguished from one another by which major constituent varies the least and the abundance of that constituent. The group consisting of Nakhla, Lafayette, Governador Valadares, and the Yamato nakhlite pairing group is characterized by low modal mesostasis and pyroxene‐olivine covariance, whereas the group consisting of the Miller Range nakhlite pairing group and Northwest Africa 5790 is characterized by low modal olivine and pyroxene‐mesostasis covariance. These two groups sample the slowest‐cooled interior portion and the chilled margin, respectively, of the nakhlite emplacement body as presently understood, and appear to be also related to recently proposed nakhlite groups independently established using compositional rather than petrographic observations. Phenocryst modal abundances vary with inferred depth in the nakhlite igneous body in a manner consistent with solidification of the nakhlite stack from dynamically sorted phenocryst‐rich magmatic crystal‐liquid mush.</subfield></datafield><datafield tag="540" ind1=" " ind2=" "><subfield code="a">Nutzungsrecht: © Published 2015. This article is a U.S. Government work and is in the public domain in the USA.</subfield></datafield><datafield tag="540" ind1=" " ind2=" "><subfield code="a">© COPYRIGHT 2015 Wiley Subscription Services, Inc.</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Meteorites</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Pyroxene</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Magma</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Velbel, Michael A</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Vicenzi, Edward P</subfield><subfield code="4">oth</subfield></datafield><datafield tag="773" ind1="0" ind2="8"><subfield code="i">Enthalten in</subfield><subfield code="t">Meteoritics & planetary science</subfield><subfield code="d">Lawrence, Kan. : Allen Press, 1996</subfield><subfield code="g">50(2015), 9, Seite 1497-1511</subfield><subfield code="w">(DE-627)193298368</subfield><subfield code="w">(DE-600)1306943-3</subfield><subfield code="w">(DE-576)060237333</subfield><subfield code="x">1086-9379</subfield><subfield code="7">nnns</subfield></datafield><datafield tag="773" ind1="1" ind2="8"><subfield code="g">volume:50</subfield><subfield code="g">year:2015</subfield><subfield code="g">number:9</subfield><subfield code="g">pages:1497-1511</subfield></datafield><datafield tag="856" ind1="4" ind2="1"><subfield code="u">http://dx.doi.org/10.1111/maps.12492</subfield><subfield code="3">Volltext</subfield></datafield><datafield tag="856" ind1="4" ind2="2"><subfield code="u">http://onlinelibrary.wiley.com/doi/10.1111/maps.12492/abstract</subfield></datafield><datafield tag="856" ind1="4" ind2="2"><subfield code="u">http://search.proquest.com/docview/1709479309</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_USEFLAG_A</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SYSFLAG_A</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_OLC</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OLC-GEO</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OLC-AST</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OPC-GGO</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OPC-AST</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_2004</subfield></datafield><datafield tag="951" ind1=" " ind2=" "><subfield code="a">AR</subfield></datafield><datafield tag="952" ind1=" " ind2=" "><subfield code="d">50</subfield><subfield code="j">2015</subfield><subfield code="e">9</subfield><subfield code="h">1497-1511</subfield></datafield></record></collection>
|
| author |
Corrigan, Catherine M |
| spellingShingle |
Corrigan, Catherine M ddc 520 misc Meteorites misc Pyroxene misc Magma Modal abundances of pyroxene, olivine, and mesostasis in nakhlites: Heterogeneity, variation, and implications for nakhlite emplacement |
| authorStr |
Corrigan, Catherine M |
| ppnlink_with_tag_str_mv |
@@773@@(DE-627)193298368 |
| format |
Article |
| dewey-ones |
520 - Astronomy & allied sciences 550 - Earth sciences |
| delete_txt_mv |
keep |
| author_role |
aut |
| collection |
OLC |
| remote_str |
false |
| illustrated |
Not Illustrated |
| issn |
1086-9379 |
| topic_title |
520 550 DNB Modal abundances of pyroxene, olivine, and mesostasis in nakhlites: Heterogeneity, variation, and implications for nakhlite emplacement Meteorites Pyroxene Magma |
| topic |
ddc 520 misc Meteorites misc Pyroxene misc Magma |
| topic_unstemmed |
ddc 520 misc Meteorites misc Pyroxene misc Magma |
| topic_browse |
ddc 520 misc Meteorites misc Pyroxene misc Magma |
| format_facet |
Aufsätze Gedruckte Aufsätze |
| format_main_str_mv |
Text Zeitschrift/Artikel |
| carriertype_str_mv |
nc |
| author2_variant |
m a v ma mav e p v ep epv |
| hierarchy_parent_title |
Meteoritics & planetary science |
| hierarchy_parent_id |
193298368 |
| dewey-tens |
520 - Astronomy 550 - Earth sciences & geology |
| hierarchy_top_title |
Meteoritics & planetary science |
| isfreeaccess_txt |
false |
| familylinks_str_mv |
(DE-627)193298368 (DE-600)1306943-3 (DE-576)060237333 |
| title |
Modal abundances of pyroxene, olivine, and mesostasis in nakhlites: Heterogeneity, variation, and implications for nakhlite emplacement |
| ctrlnum |
(DE-627)OLC1965317952 (DE-599)GBVOLC1965317952 (PRQ)c2402-94fb005993b5c1f676bc96b5853876519a8f653ce2ecf2a7149c1c644ce676300 (KEY)0042930920150000050000901497modalabundancesofpyroxeneolivineandmesostasisinnak |
| title_full |
Modal abundances of pyroxene, olivine, and mesostasis in nakhlites: Heterogeneity, variation, and implications for nakhlite emplacement |
| author_sort |
Corrigan, Catherine M |
| journal |
Meteoritics & planetary science |
| journalStr |
Meteoritics & planetary science |
| lang_code |
eng |
| isOA_bool |
false |
| dewey-hundreds |
500 - Science |
| recordtype |
marc |
| publishDateSort |
2015 |
| contenttype_str_mv |
txt |
| container_start_page |
1497 |
| author_browse |
Corrigan, Catherine M |
| container_volume |
50 |
| class |
520 550 DNB |
| format_se |
Aufsätze |
| author-letter |
Corrigan, Catherine M |
| doi_str_mv |
10.1111/maps.12492 |
| dewey-full |
520 550 |
| title_sort |
modal abundances of pyroxene, olivine, and mesostasis in nakhlites: heterogeneity, variation, and implications for nakhlite emplacement |
| title_auth |
Modal abundances of pyroxene, olivine, and mesostasis in nakhlites: Heterogeneity, variation, and implications for nakhlite emplacement |
| abstract |
Nakhlites, clinopyroxenite meteorites from Mars, share common crystallization and ejection ages, suggesting that they might have been ejected from the same place on Mars by the same ejection event (impact) and are different samples of the same thick volcanic flow unit or shallow sill. Mean modal abundances and abundance ranges of pyroxene, olivine, and mesostasis vary widely among different thin‐sections of an individual nakhlite. Lithologic heterogeneity is the main factor contributing to the observed modal‐abundance variations measured in thin‐sections prepared from different fragments of the same stone. Two groups of nakhlites are distinguished from one another by which major constituent varies the least and the abundance of that constituent. The group consisting of Nakhla, Lafayette, Governador Valadares, and the Yamato nakhlite pairing group is characterized by low modal mesostasis and pyroxene‐olivine covariance, whereas the group consisting of the Miller Range nakhlite pairing group and Northwest Africa 5790 is characterized by low modal olivine and pyroxene‐mesostasis covariance. These two groups sample the slowest‐cooled interior portion and the chilled margin, respectively, of the nakhlite emplacement body as presently understood, and appear to be also related to recently proposed nakhlite groups independently established using compositional rather than petrographic observations. Phenocryst modal abundances vary with inferred depth in the nakhlite igneous body in a manner consistent with solidification of the nakhlite stack from dynamically sorted phenocryst‐rich magmatic crystal‐liquid mush. |
| abstractGer |
Nakhlites, clinopyroxenite meteorites from Mars, share common crystallization and ejection ages, suggesting that they might have been ejected from the same place on Mars by the same ejection event (impact) and are different samples of the same thick volcanic flow unit or shallow sill. Mean modal abundances and abundance ranges of pyroxene, olivine, and mesostasis vary widely among different thin‐sections of an individual nakhlite. Lithologic heterogeneity is the main factor contributing to the observed modal‐abundance variations measured in thin‐sections prepared from different fragments of the same stone. Two groups of nakhlites are distinguished from one another by which major constituent varies the least and the abundance of that constituent. The group consisting of Nakhla, Lafayette, Governador Valadares, and the Yamato nakhlite pairing group is characterized by low modal mesostasis and pyroxene‐olivine covariance, whereas the group consisting of the Miller Range nakhlite pairing group and Northwest Africa 5790 is characterized by low modal olivine and pyroxene‐mesostasis covariance. These two groups sample the slowest‐cooled interior portion and the chilled margin, respectively, of the nakhlite emplacement body as presently understood, and appear to be also related to recently proposed nakhlite groups independently established using compositional rather than petrographic observations. Phenocryst modal abundances vary with inferred depth in the nakhlite igneous body in a manner consistent with solidification of the nakhlite stack from dynamically sorted phenocryst‐rich magmatic crystal‐liquid mush. |
| abstract_unstemmed |
Nakhlites, clinopyroxenite meteorites from Mars, share common crystallization and ejection ages, suggesting that they might have been ejected from the same place on Mars by the same ejection event (impact) and are different samples of the same thick volcanic flow unit or shallow sill. Mean modal abundances and abundance ranges of pyroxene, olivine, and mesostasis vary widely among different thin‐sections of an individual nakhlite. Lithologic heterogeneity is the main factor contributing to the observed modal‐abundance variations measured in thin‐sections prepared from different fragments of the same stone. Two groups of nakhlites are distinguished from one another by which major constituent varies the least and the abundance of that constituent. The group consisting of Nakhla, Lafayette, Governador Valadares, and the Yamato nakhlite pairing group is characterized by low modal mesostasis and pyroxene‐olivine covariance, whereas the group consisting of the Miller Range nakhlite pairing group and Northwest Africa 5790 is characterized by low modal olivine and pyroxene‐mesostasis covariance. These two groups sample the slowest‐cooled interior portion and the chilled margin, respectively, of the nakhlite emplacement body as presently understood, and appear to be also related to recently proposed nakhlite groups independently established using compositional rather than petrographic observations. Phenocryst modal abundances vary with inferred depth in the nakhlite igneous body in a manner consistent with solidification of the nakhlite stack from dynamically sorted phenocryst‐rich magmatic crystal‐liquid mush. |
| collection_details |
GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-GEO SSG-OLC-AST SSG-OPC-GGO SSG-OPC-AST GBV_ILN_2004 |
| container_issue |
9 |
| title_short |
Modal abundances of pyroxene, olivine, and mesostasis in nakhlites: Heterogeneity, variation, and implications for nakhlite emplacement |
| url |
http://dx.doi.org/10.1111/maps.12492 http://onlinelibrary.wiley.com/doi/10.1111/maps.12492/abstract http://search.proquest.com/docview/1709479309 |
| remote_bool |
false |
| author2 |
Velbel, Michael A Vicenzi, Edward P |
| author2Str |
Velbel, Michael A Vicenzi, Edward P |
| ppnlink |
193298368 |
| mediatype_str_mv |
n |
| isOA_txt |
false |
| hochschulschrift_bool |
false |
| author2_role |
oth oth |
| doi_str |
10.1111/maps.12492 |
| up_date |
2024-07-03T17:18:50.753Z |
| _version_ |
1803579168655409152 |
| fullrecord_marcxml |
<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a2200265 4500</leader><controlfield tag="001">OLC1965317952</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20230714163708.0</controlfield><controlfield tag="007">tu</controlfield><controlfield tag="008">160206s2015 xx ||||| 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1111/maps.12492</subfield><subfield code="2">doi</subfield></datafield><datafield tag="028" ind1="5" ind2="2"><subfield code="a">PQ20160617</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)OLC1965317952</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-599)GBVOLC1965317952</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(PRQ)c2402-94fb005993b5c1f676bc96b5853876519a8f653ce2ecf2a7149c1c644ce676300</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(KEY)0042930920150000050000901497modalabundancesofpyroxeneolivineandmesostasisinnak</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-627</subfield><subfield code="b">ger</subfield><subfield code="c">DE-627</subfield><subfield code="e">rakwb</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="082" ind1="0" ind2="4"><subfield code="a">520</subfield><subfield code="a">550</subfield><subfield code="q">DNB</subfield></datafield><datafield tag="100" ind1="1" ind2=" "><subfield code="a">Corrigan, Catherine M</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Modal abundances of pyroxene, olivine, and mesostasis in nakhlites: Heterogeneity, variation, and implications for nakhlite emplacement</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2015</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">ohne Hilfsmittel zu benutzen</subfield><subfield code="b">n</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Band</subfield><subfield code="b">nc</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Nakhlites, clinopyroxenite meteorites from Mars, share common crystallization and ejection ages, suggesting that they might have been ejected from the same place on Mars by the same ejection event (impact) and are different samples of the same thick volcanic flow unit or shallow sill. Mean modal abundances and abundance ranges of pyroxene, olivine, and mesostasis vary widely among different thin‐sections of an individual nakhlite. Lithologic heterogeneity is the main factor contributing to the observed modal‐abundance variations measured in thin‐sections prepared from different fragments of the same stone. Two groups of nakhlites are distinguished from one another by which major constituent varies the least and the abundance of that constituent. The group consisting of Nakhla, Lafayette, Governador Valadares, and the Yamato nakhlite pairing group is characterized by low modal mesostasis and pyroxene‐olivine covariance, whereas the group consisting of the Miller Range nakhlite pairing group and Northwest Africa 5790 is characterized by low modal olivine and pyroxene‐mesostasis covariance. These two groups sample the slowest‐cooled interior portion and the chilled margin, respectively, of the nakhlite emplacement body as presently understood, and appear to be also related to recently proposed nakhlite groups independently established using compositional rather than petrographic observations. Phenocryst modal abundances vary with inferred depth in the nakhlite igneous body in a manner consistent with solidification of the nakhlite stack from dynamically sorted phenocryst‐rich magmatic crystal‐liquid mush.</subfield></datafield><datafield tag="540" ind1=" " ind2=" "><subfield code="a">Nutzungsrecht: © Published 2015. This article is a U.S. Government work and is in the public domain in the USA.</subfield></datafield><datafield tag="540" ind1=" " ind2=" "><subfield code="a">© COPYRIGHT 2015 Wiley Subscription Services, Inc.</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Meteorites</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Pyroxene</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Magma</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Velbel, Michael A</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Vicenzi, Edward P</subfield><subfield code="4">oth</subfield></datafield><datafield tag="773" ind1="0" ind2="8"><subfield code="i">Enthalten in</subfield><subfield code="t">Meteoritics & planetary science</subfield><subfield code="d">Lawrence, Kan. : Allen Press, 1996</subfield><subfield code="g">50(2015), 9, Seite 1497-1511</subfield><subfield code="w">(DE-627)193298368</subfield><subfield code="w">(DE-600)1306943-3</subfield><subfield code="w">(DE-576)060237333</subfield><subfield code="x">1086-9379</subfield><subfield code="7">nnns</subfield></datafield><datafield tag="773" ind1="1" ind2="8"><subfield code="g">volume:50</subfield><subfield code="g">year:2015</subfield><subfield code="g">number:9</subfield><subfield code="g">pages:1497-1511</subfield></datafield><datafield tag="856" ind1="4" ind2="1"><subfield code="u">http://dx.doi.org/10.1111/maps.12492</subfield><subfield code="3">Volltext</subfield></datafield><datafield tag="856" ind1="4" ind2="2"><subfield code="u">http://onlinelibrary.wiley.com/doi/10.1111/maps.12492/abstract</subfield></datafield><datafield tag="856" ind1="4" ind2="2"><subfield code="u">http://search.proquest.com/docview/1709479309</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_USEFLAG_A</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SYSFLAG_A</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_OLC</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OLC-GEO</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OLC-AST</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OPC-GGO</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OPC-AST</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_2004</subfield></datafield><datafield tag="951" ind1=" " ind2=" "><subfield code="a">AR</subfield></datafield><datafield tag="952" ind1=" " ind2=" "><subfield code="d">50</subfield><subfield code="j">2015</subfield><subfield code="e">9</subfield><subfield code="h">1497-1511</subfield></datafield></record></collection>
|
| score |
7.399749 |