Trace elements in olivine and the petrogenesis of the intermediate, olivine‐phyric shergottite NWA 10170
Olivine‐phyric shergottites represent primitive basaltic to picritic rocks, spanning a large range of Mg# and olivine abundances. As primitive olivine‐bearing magmas are commonly representative of their mantle source on Earth, understanding the petrology and evolution of olivine‐phyric shergottites...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Howarth, Geoffrey H [verfasserIn] |
|---|
| Format: |
Artikel |
|---|---|
| Sprache: |
Englisch |
| Erschienen: |
2017 |
|---|
| Rechteinformationen: |
Nutzungsrecht: © The Meteoritical Society, 2016. |
|---|
| Übergeordnetes Werk: |
Enthalten in: Meteoritics & planetary science - Lawrence, Kan. : Allen Press, 1996, 52(2017), 2, Seite 391-409 |
|---|---|
| Übergeordnetes Werk: |
volume:52 ; year:2017 ; number:2 ; pages:391-409 |
| Links: |
|---|
| DOI / URN: |
10.1111/maps.12799 |
|---|
| Katalog-ID: |
OLC1990478832 |
|---|
| LEADER | 01000caa a2200265 4500 | ||
|---|---|---|---|
| 001 | OLC1990478832 | ||
| 003 | DE-627 | ||
| 005 | 20230715031902.0 | ||
| 007 | tu | ||
| 008 | 170303s2017 xx ||||| 00| ||eng c | ||
| 024 | 7 | |a 10.1111/maps.12799 |2 doi | |
| 028 | 5 | 2 | |a PQ20170301 |
| 035 | |a (DE-627)OLC1990478832 | ||
| 035 | |a (DE-599)GBVOLC1990478832 | ||
| 035 | |a (PRQ)c1299-422b4bb8a6b9ba093d0ec6d4de4617daab0310df4eba81cf7d75a170ff4fd750 | ||
| 035 | |a (KEY)0042930920170000052000200391traceelementsinolivineandthepetrogenesisoftheinter | ||
| 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 Howarth, Geoffrey H |e verfasserin |4 aut | |
| 245 | 1 | 0 | |a Trace elements in olivine and the petrogenesis of the intermediate, olivine‐phyric shergottite NWA 10170 |
| 264 | 1 | |c 2017 | |
| 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 Olivine‐phyric shergottites represent primitive basaltic to picritic rocks, spanning a large range of Mg# and olivine abundances. As primitive olivine‐bearing magmas are commonly representative of their mantle source on Earth, understanding the petrology and evolution of olivine‐phyric shergottites is critical in our understanding of Martian mantle compositions. We present data for the olivine‐phyric shergottite Northwest Africa ( NWA ) 10170 to constrain the petrology with specific implications for magma plumbing‐system dynamics. The calculated oxygen fugacity and bulk‐rock REE concentrations (based on modal abundance) are consistent with a geochemically intermediate classification for NWA 10170, and overall similarity with NWA 6234. In addition, we present trace element data using laser ablation ICP ‐ MS for coarse‐grained olivine cores, and compare these data with terrestrial and Martian data sets. The olivines in NWA 10170 contain cores with compositions of Fo 77 that evolve to rims with composition of Fo 58 , and are characterized by cores with low Ni contents (400–600 ppm). Nickel is compatible in olivine and such low Ni content for olivine cores in NWA 10170 suggests either early‐stage fractionation and loss of olivine from the magma in a staging chamber at depth, or that Martian magmas have lower Ni than terrestrial magmas. We suggest that both are true in this case. Therefore, the magma does not represent a primary mantle melt, but rather has undergone 10–15% fractionation in a staging chamber prior to extrusion/intrusion at the surface of Mars. This further implies that careful evaluation of not only the Mg# but also the trace element concentrations of olivine needs to be conducted to evaluate pristine mantle melts versus those that have fractionated olivine (±pyroxene and oxide minerals) in staging chambers. | ||
| 540 | |a Nutzungsrecht: © The Meteoritical Society, 2016. | ||
| 700 | 1 | |a Udry, Arya |4 oth | |
| 773 | 0 | 8 | |i Enthalten in |t Meteoritics & planetary science |d Lawrence, Kan. : Allen Press, 1996 |g 52(2017), 2, Seite 391-409 |w (DE-627)193298368 |w (DE-600)1306943-3 |w (DE-576)060237333 |x 1086-9379 |7 nnns |
| 773 | 1 | 8 | |g volume:52 |g year:2017 |g number:2 |g pages:391-409 |
| 856 | 4 | 1 | |u http://dx.doi.org/10.1111/maps.12799 |3 Volltext |
| 856 | 4 | 2 | |u http://onlinelibrary.wiley.com/doi/10.1111/maps.12799/abstract |
| 856 | 4 | 2 | |u http://search.proquest.com/docview/1865614146 |
| 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 52 |j 2017 |e 2 |h 391-409 | ||
| author_variant |
g h h gh ghh |
|---|---|
| matchkey_str |
article:10869379:2017----::rceeetioiienteergnssfhitreitoiieh |
| hierarchy_sort_str |
2017 |
| publishDate |
2017 |
| allfields |
10.1111/maps.12799 doi PQ20170301 (DE-627)OLC1990478832 (DE-599)GBVOLC1990478832 (PRQ)c1299-422b4bb8a6b9ba093d0ec6d4de4617daab0310df4eba81cf7d75a170ff4fd750 (KEY)0042930920170000052000200391traceelementsinolivineandthepetrogenesisoftheinter DE-627 ger DE-627 rakwb eng 520 550 DNB Howarth, Geoffrey H verfasserin aut Trace elements in olivine and the petrogenesis of the intermediate, olivine‐phyric shergottite NWA 10170 2017 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Olivine‐phyric shergottites represent primitive basaltic to picritic rocks, spanning a large range of Mg# and olivine abundances. As primitive olivine‐bearing magmas are commonly representative of their mantle source on Earth, understanding the petrology and evolution of olivine‐phyric shergottites is critical in our understanding of Martian mantle compositions. We present data for the olivine‐phyric shergottite Northwest Africa ( NWA ) 10170 to constrain the petrology with specific implications for magma plumbing‐system dynamics. The calculated oxygen fugacity and bulk‐rock REE concentrations (based on modal abundance) are consistent with a geochemically intermediate classification for NWA 10170, and overall similarity with NWA 6234. In addition, we present trace element data using laser ablation ICP ‐ MS for coarse‐grained olivine cores, and compare these data with terrestrial and Martian data sets. The olivines in NWA 10170 contain cores with compositions of Fo 77 that evolve to rims with composition of Fo 58 , and are characterized by cores with low Ni contents (400–600 ppm). Nickel is compatible in olivine and such low Ni content for olivine cores in NWA 10170 suggests either early‐stage fractionation and loss of olivine from the magma in a staging chamber at depth, or that Martian magmas have lower Ni than terrestrial magmas. We suggest that both are true in this case. Therefore, the magma does not represent a primary mantle melt, but rather has undergone 10–15% fractionation in a staging chamber prior to extrusion/intrusion at the surface of Mars. This further implies that careful evaluation of not only the Mg# but also the trace element concentrations of olivine needs to be conducted to evaluate pristine mantle melts versus those that have fractionated olivine (±pyroxene and oxide minerals) in staging chambers. Nutzungsrecht: © The Meteoritical Society, 2016. Udry, Arya oth Enthalten in Meteoritics & planetary science Lawrence, Kan. : Allen Press, 1996 52(2017), 2, Seite 391-409 (DE-627)193298368 (DE-600)1306943-3 (DE-576)060237333 1086-9379 nnns volume:52 year:2017 number:2 pages:391-409 http://dx.doi.org/10.1111/maps.12799 Volltext http://onlinelibrary.wiley.com/doi/10.1111/maps.12799/abstract http://search.proquest.com/docview/1865614146 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-GEO SSG-OLC-AST SSG-OPC-GGO SSG-OPC-AST GBV_ILN_2004 AR 52 2017 2 391-409 |
| spelling |
10.1111/maps.12799 doi PQ20170301 (DE-627)OLC1990478832 (DE-599)GBVOLC1990478832 (PRQ)c1299-422b4bb8a6b9ba093d0ec6d4de4617daab0310df4eba81cf7d75a170ff4fd750 (KEY)0042930920170000052000200391traceelementsinolivineandthepetrogenesisoftheinter DE-627 ger DE-627 rakwb eng 520 550 DNB Howarth, Geoffrey H verfasserin aut Trace elements in olivine and the petrogenesis of the intermediate, olivine‐phyric shergottite NWA 10170 2017 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Olivine‐phyric shergottites represent primitive basaltic to picritic rocks, spanning a large range of Mg# and olivine abundances. As primitive olivine‐bearing magmas are commonly representative of their mantle source on Earth, understanding the petrology and evolution of olivine‐phyric shergottites is critical in our understanding of Martian mantle compositions. We present data for the olivine‐phyric shergottite Northwest Africa ( NWA ) 10170 to constrain the petrology with specific implications for magma plumbing‐system dynamics. The calculated oxygen fugacity and bulk‐rock REE concentrations (based on modal abundance) are consistent with a geochemically intermediate classification for NWA 10170, and overall similarity with NWA 6234. In addition, we present trace element data using laser ablation ICP ‐ MS for coarse‐grained olivine cores, and compare these data with terrestrial and Martian data sets. The olivines in NWA 10170 contain cores with compositions of Fo 77 that evolve to rims with composition of Fo 58 , and are characterized by cores with low Ni contents (400–600 ppm). Nickel is compatible in olivine and such low Ni content for olivine cores in NWA 10170 suggests either early‐stage fractionation and loss of olivine from the magma in a staging chamber at depth, or that Martian magmas have lower Ni than terrestrial magmas. We suggest that both are true in this case. Therefore, the magma does not represent a primary mantle melt, but rather has undergone 10–15% fractionation in a staging chamber prior to extrusion/intrusion at the surface of Mars. This further implies that careful evaluation of not only the Mg# but also the trace element concentrations of olivine needs to be conducted to evaluate pristine mantle melts versus those that have fractionated olivine (±pyroxene and oxide minerals) in staging chambers. Nutzungsrecht: © The Meteoritical Society, 2016. Udry, Arya oth Enthalten in Meteoritics & planetary science Lawrence, Kan. : Allen Press, 1996 52(2017), 2, Seite 391-409 (DE-627)193298368 (DE-600)1306943-3 (DE-576)060237333 1086-9379 nnns volume:52 year:2017 number:2 pages:391-409 http://dx.doi.org/10.1111/maps.12799 Volltext http://onlinelibrary.wiley.com/doi/10.1111/maps.12799/abstract http://search.proquest.com/docview/1865614146 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-GEO SSG-OLC-AST SSG-OPC-GGO SSG-OPC-AST GBV_ILN_2004 AR 52 2017 2 391-409 |
| allfields_unstemmed |
10.1111/maps.12799 doi PQ20170301 (DE-627)OLC1990478832 (DE-599)GBVOLC1990478832 (PRQ)c1299-422b4bb8a6b9ba093d0ec6d4de4617daab0310df4eba81cf7d75a170ff4fd750 (KEY)0042930920170000052000200391traceelementsinolivineandthepetrogenesisoftheinter DE-627 ger DE-627 rakwb eng 520 550 DNB Howarth, Geoffrey H verfasserin aut Trace elements in olivine and the petrogenesis of the intermediate, olivine‐phyric shergottite NWA 10170 2017 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Olivine‐phyric shergottites represent primitive basaltic to picritic rocks, spanning a large range of Mg# and olivine abundances. As primitive olivine‐bearing magmas are commonly representative of their mantle source on Earth, understanding the petrology and evolution of olivine‐phyric shergottites is critical in our understanding of Martian mantle compositions. We present data for the olivine‐phyric shergottite Northwest Africa ( NWA ) 10170 to constrain the petrology with specific implications for magma plumbing‐system dynamics. The calculated oxygen fugacity and bulk‐rock REE concentrations (based on modal abundance) are consistent with a geochemically intermediate classification for NWA 10170, and overall similarity with NWA 6234. In addition, we present trace element data using laser ablation ICP ‐ MS for coarse‐grained olivine cores, and compare these data with terrestrial and Martian data sets. The olivines in NWA 10170 contain cores with compositions of Fo 77 that evolve to rims with composition of Fo 58 , and are characterized by cores with low Ni contents (400–600 ppm). Nickel is compatible in olivine and such low Ni content for olivine cores in NWA 10170 suggests either early‐stage fractionation and loss of olivine from the magma in a staging chamber at depth, or that Martian magmas have lower Ni than terrestrial magmas. We suggest that both are true in this case. Therefore, the magma does not represent a primary mantle melt, but rather has undergone 10–15% fractionation in a staging chamber prior to extrusion/intrusion at the surface of Mars. This further implies that careful evaluation of not only the Mg# but also the trace element concentrations of olivine needs to be conducted to evaluate pristine mantle melts versus those that have fractionated olivine (±pyroxene and oxide minerals) in staging chambers. Nutzungsrecht: © The Meteoritical Society, 2016. Udry, Arya oth Enthalten in Meteoritics & planetary science Lawrence, Kan. : Allen Press, 1996 52(2017), 2, Seite 391-409 (DE-627)193298368 (DE-600)1306943-3 (DE-576)060237333 1086-9379 nnns volume:52 year:2017 number:2 pages:391-409 http://dx.doi.org/10.1111/maps.12799 Volltext http://onlinelibrary.wiley.com/doi/10.1111/maps.12799/abstract http://search.proquest.com/docview/1865614146 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-GEO SSG-OLC-AST SSG-OPC-GGO SSG-OPC-AST GBV_ILN_2004 AR 52 2017 2 391-409 |
| allfieldsGer |
10.1111/maps.12799 doi PQ20170301 (DE-627)OLC1990478832 (DE-599)GBVOLC1990478832 (PRQ)c1299-422b4bb8a6b9ba093d0ec6d4de4617daab0310df4eba81cf7d75a170ff4fd750 (KEY)0042930920170000052000200391traceelementsinolivineandthepetrogenesisoftheinter DE-627 ger DE-627 rakwb eng 520 550 DNB Howarth, Geoffrey H verfasserin aut Trace elements in olivine and the petrogenesis of the intermediate, olivine‐phyric shergottite NWA 10170 2017 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Olivine‐phyric shergottites represent primitive basaltic to picritic rocks, spanning a large range of Mg# and olivine abundances. As primitive olivine‐bearing magmas are commonly representative of their mantle source on Earth, understanding the petrology and evolution of olivine‐phyric shergottites is critical in our understanding of Martian mantle compositions. We present data for the olivine‐phyric shergottite Northwest Africa ( NWA ) 10170 to constrain the petrology with specific implications for magma plumbing‐system dynamics. The calculated oxygen fugacity and bulk‐rock REE concentrations (based on modal abundance) are consistent with a geochemically intermediate classification for NWA 10170, and overall similarity with NWA 6234. In addition, we present trace element data using laser ablation ICP ‐ MS for coarse‐grained olivine cores, and compare these data with terrestrial and Martian data sets. The olivines in NWA 10170 contain cores with compositions of Fo 77 that evolve to rims with composition of Fo 58 , and are characterized by cores with low Ni contents (400–600 ppm). Nickel is compatible in olivine and such low Ni content for olivine cores in NWA 10170 suggests either early‐stage fractionation and loss of olivine from the magma in a staging chamber at depth, or that Martian magmas have lower Ni than terrestrial magmas. We suggest that both are true in this case. Therefore, the magma does not represent a primary mantle melt, but rather has undergone 10–15% fractionation in a staging chamber prior to extrusion/intrusion at the surface of Mars. This further implies that careful evaluation of not only the Mg# but also the trace element concentrations of olivine needs to be conducted to evaluate pristine mantle melts versus those that have fractionated olivine (±pyroxene and oxide minerals) in staging chambers. Nutzungsrecht: © The Meteoritical Society, 2016. Udry, Arya oth Enthalten in Meteoritics & planetary science Lawrence, Kan. : Allen Press, 1996 52(2017), 2, Seite 391-409 (DE-627)193298368 (DE-600)1306943-3 (DE-576)060237333 1086-9379 nnns volume:52 year:2017 number:2 pages:391-409 http://dx.doi.org/10.1111/maps.12799 Volltext http://onlinelibrary.wiley.com/doi/10.1111/maps.12799/abstract http://search.proquest.com/docview/1865614146 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-GEO SSG-OLC-AST SSG-OPC-GGO SSG-OPC-AST GBV_ILN_2004 AR 52 2017 2 391-409 |
| allfieldsSound |
10.1111/maps.12799 doi PQ20170301 (DE-627)OLC1990478832 (DE-599)GBVOLC1990478832 (PRQ)c1299-422b4bb8a6b9ba093d0ec6d4de4617daab0310df4eba81cf7d75a170ff4fd750 (KEY)0042930920170000052000200391traceelementsinolivineandthepetrogenesisoftheinter DE-627 ger DE-627 rakwb eng 520 550 DNB Howarth, Geoffrey H verfasserin aut Trace elements in olivine and the petrogenesis of the intermediate, olivine‐phyric shergottite NWA 10170 2017 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Olivine‐phyric shergottites represent primitive basaltic to picritic rocks, spanning a large range of Mg# and olivine abundances. As primitive olivine‐bearing magmas are commonly representative of their mantle source on Earth, understanding the petrology and evolution of olivine‐phyric shergottites is critical in our understanding of Martian mantle compositions. We present data for the olivine‐phyric shergottite Northwest Africa ( NWA ) 10170 to constrain the petrology with specific implications for magma plumbing‐system dynamics. The calculated oxygen fugacity and bulk‐rock REE concentrations (based on modal abundance) are consistent with a geochemically intermediate classification for NWA 10170, and overall similarity with NWA 6234. In addition, we present trace element data using laser ablation ICP ‐ MS for coarse‐grained olivine cores, and compare these data with terrestrial and Martian data sets. The olivines in NWA 10170 contain cores with compositions of Fo 77 that evolve to rims with composition of Fo 58 , and are characterized by cores with low Ni contents (400–600 ppm). Nickel is compatible in olivine and such low Ni content for olivine cores in NWA 10170 suggests either early‐stage fractionation and loss of olivine from the magma in a staging chamber at depth, or that Martian magmas have lower Ni than terrestrial magmas. We suggest that both are true in this case. Therefore, the magma does not represent a primary mantle melt, but rather has undergone 10–15% fractionation in a staging chamber prior to extrusion/intrusion at the surface of Mars. This further implies that careful evaluation of not only the Mg# but also the trace element concentrations of olivine needs to be conducted to evaluate pristine mantle melts versus those that have fractionated olivine (±pyroxene and oxide minerals) in staging chambers. Nutzungsrecht: © The Meteoritical Society, 2016. Udry, Arya oth Enthalten in Meteoritics & planetary science Lawrence, Kan. : Allen Press, 1996 52(2017), 2, Seite 391-409 (DE-627)193298368 (DE-600)1306943-3 (DE-576)060237333 1086-9379 nnns volume:52 year:2017 number:2 pages:391-409 http://dx.doi.org/10.1111/maps.12799 Volltext http://onlinelibrary.wiley.com/doi/10.1111/maps.12799/abstract http://search.proquest.com/docview/1865614146 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-GEO SSG-OLC-AST SSG-OPC-GGO SSG-OPC-AST GBV_ILN_2004 AR 52 2017 2 391-409 |
| language |
English |
| source |
Enthalten in Meteoritics & planetary science 52(2017), 2, Seite 391-409 volume:52 year:2017 number:2 pages:391-409 |
| sourceStr |
Enthalten in Meteoritics & planetary science 52(2017), 2, Seite 391-409 volume:52 year:2017 number:2 pages:391-409 |
| format_phy_str_mv |
Article |
| institution |
findex.gbv.de |
| dewey-raw |
520 |
| isfreeaccess_bool |
false |
| container_title |
Meteoritics & planetary science |
| authorswithroles_txt_mv |
Howarth, Geoffrey H @@aut@@ Udry, Arya @@oth@@ |
| publishDateDaySort_date |
2017-01-01T00:00:00Z |
| hierarchy_top_id |
193298368 |
| dewey-sort |
3520 |
| id |
OLC1990478832 |
| 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">OLC1990478832</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20230715031902.0</controlfield><controlfield tag="007">tu</controlfield><controlfield tag="008">170303s2017 xx ||||| 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1111/maps.12799</subfield><subfield code="2">doi</subfield></datafield><datafield tag="028" ind1="5" ind2="2"><subfield code="a">PQ20170301</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)OLC1990478832</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-599)GBVOLC1990478832</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(PRQ)c1299-422b4bb8a6b9ba093d0ec6d4de4617daab0310df4eba81cf7d75a170ff4fd750</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(KEY)0042930920170000052000200391traceelementsinolivineandthepetrogenesisoftheinter</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">Howarth, Geoffrey H</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Trace elements in olivine and the petrogenesis of the intermediate, olivine‐phyric shergottite NWA 10170</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2017</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">Olivine‐phyric shergottites represent primitive basaltic to picritic rocks, spanning a large range of Mg# and olivine abundances. As primitive olivine‐bearing magmas are commonly representative of their mantle source on Earth, understanding the petrology and evolution of olivine‐phyric shergottites is critical in our understanding of Martian mantle compositions. We present data for the olivine‐phyric shergottite Northwest Africa ( NWA ) 10170 to constrain the petrology with specific implications for magma plumbing‐system dynamics. The calculated oxygen fugacity and bulk‐rock REE concentrations (based on modal abundance) are consistent with a geochemically intermediate classification for NWA 10170, and overall similarity with NWA 6234. In addition, we present trace element data using laser ablation ICP ‐ MS for coarse‐grained olivine cores, and compare these data with terrestrial and Martian data sets. The olivines in NWA 10170 contain cores with compositions of Fo 77 that evolve to rims with composition of Fo 58 , and are characterized by cores with low Ni contents (400–600 ppm). Nickel is compatible in olivine and such low Ni content for olivine cores in NWA 10170 suggests either early‐stage fractionation and loss of olivine from the magma in a staging chamber at depth, or that Martian magmas have lower Ni than terrestrial magmas. We suggest that both are true in this case. Therefore, the magma does not represent a primary mantle melt, but rather has undergone 10–15% fractionation in a staging chamber prior to extrusion/intrusion at the surface of Mars. This further implies that careful evaluation of not only the Mg# but also the trace element concentrations of olivine needs to be conducted to evaluate pristine mantle melts versus those that have fractionated olivine (±pyroxene and oxide minerals) in staging chambers.</subfield></datafield><datafield tag="540" ind1=" " ind2=" "><subfield code="a">Nutzungsrecht: © The Meteoritical Society, 2016.</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Udry, Arya</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">52(2017), 2, Seite 391-409</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:52</subfield><subfield code="g">year:2017</subfield><subfield code="g">number:2</subfield><subfield code="g">pages:391-409</subfield></datafield><datafield tag="856" ind1="4" ind2="1"><subfield code="u">http://dx.doi.org/10.1111/maps.12799</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.12799/abstract</subfield></datafield><datafield tag="856" ind1="4" ind2="2"><subfield code="u">http://search.proquest.com/docview/1865614146</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">52</subfield><subfield code="j">2017</subfield><subfield code="e">2</subfield><subfield code="h">391-409</subfield></datafield></record></collection>
|
| author |
Howarth, Geoffrey H |
| spellingShingle |
Howarth, Geoffrey H ddc 520 Trace elements in olivine and the petrogenesis of the intermediate, olivine‐phyric shergottite NWA 10170 |
| authorStr |
Howarth, Geoffrey H |
| 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 Trace elements in olivine and the petrogenesis of the intermediate, olivine‐phyric shergottite NWA 10170 |
| topic |
ddc 520 |
| topic_unstemmed |
ddc 520 |
| topic_browse |
ddc 520 |
| format_facet |
Aufsätze Gedruckte Aufsätze |
| format_main_str_mv |
Text Zeitschrift/Artikel |
| carriertype_str_mv |
nc |
| author2_variant |
a u au |
| 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 |
Trace elements in olivine and the petrogenesis of the intermediate, olivine‐phyric shergottite NWA 10170 |
| ctrlnum |
(DE-627)OLC1990478832 (DE-599)GBVOLC1990478832 (PRQ)c1299-422b4bb8a6b9ba093d0ec6d4de4617daab0310df4eba81cf7d75a170ff4fd750 (KEY)0042930920170000052000200391traceelementsinolivineandthepetrogenesisoftheinter |
| title_full |
Trace elements in olivine and the petrogenesis of the intermediate, olivine‐phyric shergottite NWA 10170 |
| author_sort |
Howarth, Geoffrey H |
| journal |
Meteoritics & planetary science |
| journalStr |
Meteoritics & planetary science |
| lang_code |
eng |
| isOA_bool |
false |
| dewey-hundreds |
500 - Science |
| recordtype |
marc |
| publishDateSort |
2017 |
| contenttype_str_mv |
txt |
| container_start_page |
391 |
| author_browse |
Howarth, Geoffrey H |
| container_volume |
52 |
| class |
520 550 DNB |
| format_se |
Aufsätze |
| author-letter |
Howarth, Geoffrey H |
| doi_str_mv |
10.1111/maps.12799 |
| dewey-full |
520 550 |
| title_sort |
trace elements in olivine and the petrogenesis of the intermediate, olivine‐phyric shergottite nwa 10170 |
| title_auth |
Trace elements in olivine and the petrogenesis of the intermediate, olivine‐phyric shergottite NWA 10170 |
| abstract |
Olivine‐phyric shergottites represent primitive basaltic to picritic rocks, spanning a large range of Mg# and olivine abundances. As primitive olivine‐bearing magmas are commonly representative of their mantle source on Earth, understanding the petrology and evolution of olivine‐phyric shergottites is critical in our understanding of Martian mantle compositions. We present data for the olivine‐phyric shergottite Northwest Africa ( NWA ) 10170 to constrain the petrology with specific implications for magma plumbing‐system dynamics. The calculated oxygen fugacity and bulk‐rock REE concentrations (based on modal abundance) are consistent with a geochemically intermediate classification for NWA 10170, and overall similarity with NWA 6234. In addition, we present trace element data using laser ablation ICP ‐ MS for coarse‐grained olivine cores, and compare these data with terrestrial and Martian data sets. The olivines in NWA 10170 contain cores with compositions of Fo 77 that evolve to rims with composition of Fo 58 , and are characterized by cores with low Ni contents (400–600 ppm). Nickel is compatible in olivine and such low Ni content for olivine cores in NWA 10170 suggests either early‐stage fractionation and loss of olivine from the magma in a staging chamber at depth, or that Martian magmas have lower Ni than terrestrial magmas. We suggest that both are true in this case. Therefore, the magma does not represent a primary mantle melt, but rather has undergone 10–15% fractionation in a staging chamber prior to extrusion/intrusion at the surface of Mars. This further implies that careful evaluation of not only the Mg# but also the trace element concentrations of olivine needs to be conducted to evaluate pristine mantle melts versus those that have fractionated olivine (±pyroxene and oxide minerals) in staging chambers. |
| abstractGer |
Olivine‐phyric shergottites represent primitive basaltic to picritic rocks, spanning a large range of Mg# and olivine abundances. As primitive olivine‐bearing magmas are commonly representative of their mantle source on Earth, understanding the petrology and evolution of olivine‐phyric shergottites is critical in our understanding of Martian mantle compositions. We present data for the olivine‐phyric shergottite Northwest Africa ( NWA ) 10170 to constrain the petrology with specific implications for magma plumbing‐system dynamics. The calculated oxygen fugacity and bulk‐rock REE concentrations (based on modal abundance) are consistent with a geochemically intermediate classification for NWA 10170, and overall similarity with NWA 6234. In addition, we present trace element data using laser ablation ICP ‐ MS for coarse‐grained olivine cores, and compare these data with terrestrial and Martian data sets. The olivines in NWA 10170 contain cores with compositions of Fo 77 that evolve to rims with composition of Fo 58 , and are characterized by cores with low Ni contents (400–600 ppm). Nickel is compatible in olivine and such low Ni content for olivine cores in NWA 10170 suggests either early‐stage fractionation and loss of olivine from the magma in a staging chamber at depth, or that Martian magmas have lower Ni than terrestrial magmas. We suggest that both are true in this case. Therefore, the magma does not represent a primary mantle melt, but rather has undergone 10–15% fractionation in a staging chamber prior to extrusion/intrusion at the surface of Mars. This further implies that careful evaluation of not only the Mg# but also the trace element concentrations of olivine needs to be conducted to evaluate pristine mantle melts versus those that have fractionated olivine (±pyroxene and oxide minerals) in staging chambers. |
| abstract_unstemmed |
Olivine‐phyric shergottites represent primitive basaltic to picritic rocks, spanning a large range of Mg# and olivine abundances. As primitive olivine‐bearing magmas are commonly representative of their mantle source on Earth, understanding the petrology and evolution of olivine‐phyric shergottites is critical in our understanding of Martian mantle compositions. We present data for the olivine‐phyric shergottite Northwest Africa ( NWA ) 10170 to constrain the petrology with specific implications for magma plumbing‐system dynamics. The calculated oxygen fugacity and bulk‐rock REE concentrations (based on modal abundance) are consistent with a geochemically intermediate classification for NWA 10170, and overall similarity with NWA 6234. In addition, we present trace element data using laser ablation ICP ‐ MS for coarse‐grained olivine cores, and compare these data with terrestrial and Martian data sets. The olivines in NWA 10170 contain cores with compositions of Fo 77 that evolve to rims with composition of Fo 58 , and are characterized by cores with low Ni contents (400–600 ppm). Nickel is compatible in olivine and such low Ni content for olivine cores in NWA 10170 suggests either early‐stage fractionation and loss of olivine from the magma in a staging chamber at depth, or that Martian magmas have lower Ni than terrestrial magmas. We suggest that both are true in this case. Therefore, the magma does not represent a primary mantle melt, but rather has undergone 10–15% fractionation in a staging chamber prior to extrusion/intrusion at the surface of Mars. This further implies that careful evaluation of not only the Mg# but also the trace element concentrations of olivine needs to be conducted to evaluate pristine mantle melts versus those that have fractionated olivine (±pyroxene and oxide minerals) in staging chambers. |
| 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 |
2 |
| title_short |
Trace elements in olivine and the petrogenesis of the intermediate, olivine‐phyric shergottite NWA 10170 |
| url |
http://dx.doi.org/10.1111/maps.12799 http://onlinelibrary.wiley.com/doi/10.1111/maps.12799/abstract http://search.proquest.com/docview/1865614146 |
| remote_bool |
false |
| author2 |
Udry, Arya |
| author2Str |
Udry, Arya |
| ppnlink |
193298368 |
| mediatype_str_mv |
n |
| isOA_txt |
false |
| hochschulschrift_bool |
false |
| author2_role |
oth |
| doi_str |
10.1111/maps.12799 |
| up_date |
2024-07-04T01:05:06.208Z |
| _version_ |
1803608503047159808 |
| 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">OLC1990478832</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20230715031902.0</controlfield><controlfield tag="007">tu</controlfield><controlfield tag="008">170303s2017 xx ||||| 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1111/maps.12799</subfield><subfield code="2">doi</subfield></datafield><datafield tag="028" ind1="5" ind2="2"><subfield code="a">PQ20170301</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)OLC1990478832</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-599)GBVOLC1990478832</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(PRQ)c1299-422b4bb8a6b9ba093d0ec6d4de4617daab0310df4eba81cf7d75a170ff4fd750</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(KEY)0042930920170000052000200391traceelementsinolivineandthepetrogenesisoftheinter</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">Howarth, Geoffrey H</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Trace elements in olivine and the petrogenesis of the intermediate, olivine‐phyric shergottite NWA 10170</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2017</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">Olivine‐phyric shergottites represent primitive basaltic to picritic rocks, spanning a large range of Mg# and olivine abundances. As primitive olivine‐bearing magmas are commonly representative of their mantle source on Earth, understanding the petrology and evolution of olivine‐phyric shergottites is critical in our understanding of Martian mantle compositions. We present data for the olivine‐phyric shergottite Northwest Africa ( NWA ) 10170 to constrain the petrology with specific implications for magma plumbing‐system dynamics. The calculated oxygen fugacity and bulk‐rock REE concentrations (based on modal abundance) are consistent with a geochemically intermediate classification for NWA 10170, and overall similarity with NWA 6234. In addition, we present trace element data using laser ablation ICP ‐ MS for coarse‐grained olivine cores, and compare these data with terrestrial and Martian data sets. The olivines in NWA 10170 contain cores with compositions of Fo 77 that evolve to rims with composition of Fo 58 , and are characterized by cores with low Ni contents (400–600 ppm). Nickel is compatible in olivine and such low Ni content for olivine cores in NWA 10170 suggests either early‐stage fractionation and loss of olivine from the magma in a staging chamber at depth, or that Martian magmas have lower Ni than terrestrial magmas. We suggest that both are true in this case. Therefore, the magma does not represent a primary mantle melt, but rather has undergone 10–15% fractionation in a staging chamber prior to extrusion/intrusion at the surface of Mars. This further implies that careful evaluation of not only the Mg# but also the trace element concentrations of olivine needs to be conducted to evaluate pristine mantle melts versus those that have fractionated olivine (±pyroxene and oxide minerals) in staging chambers.</subfield></datafield><datafield tag="540" ind1=" " ind2=" "><subfield code="a">Nutzungsrecht: © The Meteoritical Society, 2016.</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Udry, Arya</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">52(2017), 2, Seite 391-409</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:52</subfield><subfield code="g">year:2017</subfield><subfield code="g">number:2</subfield><subfield code="g">pages:391-409</subfield></datafield><datafield tag="856" ind1="4" ind2="1"><subfield code="u">http://dx.doi.org/10.1111/maps.12799</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.12799/abstract</subfield></datafield><datafield tag="856" ind1="4" ind2="2"><subfield code="u">http://search.proquest.com/docview/1865614146</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">52</subfield><subfield code="j">2017</subfield><subfield code="e">2</subfield><subfield code="h">391-409</subfield></datafield></record></collection>
|
| score |
7.400899 |