The non-igneous genesis of angrites: Support from trace element distribution between phases in D’Orbigny
- Autores
- Varela, Maria Eugenia; Kurat, Gero; Zinner, Ernst; Hoppe, Peter; Ntaflos, T.; Nazarov, M.
- Año de publicación
- 2005
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- D'Orbigny is an exceptional angrite. Chemically, it resembles other angrites such as Asuka-881371, Sahara 99555, Lewis Cliff (LEW) 87051, and LEW 86010, but its structure and texture are peculiar. It has a compact and porous lithology, abundant glasses, augite-bearing druses, and chemical and mineralogical properties that are highly unusual for igneous rocks. Our previous studies led us to a new view on angrites: they can possibly be considered as CAIs that grew to larger sizes than the ones we know from carbonaceous chondrites. Thus, angrites may bear a record of rare and special conditions in some part of the early solar nebula. Here we report trace element contents of D'Orbigny phases. Trace element data were obtained from both the porous and the compact part of this meteorite. We have confronted our results with the popular igneous genetic model. According to this model, if all phases of D'Orbigny crystallized from the same system, as an igneous origin implies, a record of this genesis should be expressed in the distribution of trace elements among early and late phases. Our results show that the trace element distribution of the two contemporaneous phases olivine and plagioclase, which form the backbone of the rock, seem to require liquids of different composition. Abundances of highly incompatible elements in all olivines, including the megacrysts, indicate disequilibrium with the bulk rock and suggest liquids very rich in these elements (>10,000 x CI), which is much richer than any fractional crystallization could possibly produce. In addition, trace element contents of late phases are incompatible with formation from the bulk system's residual melt. These results add additional severe constraints to the many conflicts that existed previously between an igneous model for the origin of angrites and the mineralogical and chemical observations. This new trace element content data, reported here, corroborate our previous results based on the shape, structure, mineralogy, chemical, and isotopic data of the whole meteorite, as well as on a petrographic and chemical composition study of all types of glasses and give strength to a new genetic model that postulates that D'Orbigny (and possibly all angrites) could have formed in the solar nebula under changing redox conditions, more akin to chondritic constituents (e.g., CAIs) than to planetary differentiated rock.
Fil: Varela, Maria Eugenia. Universidad Nacional del Sur; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Bahía Blanca; Argentina
Fil: Kurat, Gero. Universidad de Viena; Austria
Fil: Zinner, Ernst. University of Washington; Estados Unidos
Fil: Hoppe, Peter. Institut Max Planck fuer Bioanorganische Chemie; Alemania
Fil: Ntaflos, T.. Universidad de Viena; Austria
Fil: Nazarov, M.. Vernadsky Institute; Rusia - Materia
-
angrites
condensacion
genesis
D´Orbigny - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/214801
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The non-igneous genesis of angrites: Support from trace element distribution between phases in D’OrbignyVarela, Maria EugeniaKurat, GeroZinner, ErnstHoppe, PeterNtaflos, T.Nazarov, M.angritescondensaciongenesisD´Orbignyhttps://purl.org/becyt/ford/1.5https://purl.org/becyt/ford/1D'Orbigny is an exceptional angrite. Chemically, it resembles other angrites such as Asuka-881371, Sahara 99555, Lewis Cliff (LEW) 87051, and LEW 86010, but its structure and texture are peculiar. It has a compact and porous lithology, abundant glasses, augite-bearing druses, and chemical and mineralogical properties that are highly unusual for igneous rocks. Our previous studies led us to a new view on angrites: they can possibly be considered as CAIs that grew to larger sizes than the ones we know from carbonaceous chondrites. Thus, angrites may bear a record of rare and special conditions in some part of the early solar nebula. Here we report trace element contents of D'Orbigny phases. Trace element data were obtained from both the porous and the compact part of this meteorite. We have confronted our results with the popular igneous genetic model. According to this model, if all phases of D'Orbigny crystallized from the same system, as an igneous origin implies, a record of this genesis should be expressed in the distribution of trace elements among early and late phases. Our results show that the trace element distribution of the two contemporaneous phases olivine and plagioclase, which form the backbone of the rock, seem to require liquids of different composition. Abundances of highly incompatible elements in all olivines, including the megacrysts, indicate disequilibrium with the bulk rock and suggest liquids very rich in these elements (>10,000 x CI), which is much richer than any fractional crystallization could possibly produce. In addition, trace element contents of late phases are incompatible with formation from the bulk system's residual melt. These results add additional severe constraints to the many conflicts that existed previously between an igneous model for the origin of angrites and the mineralogical and chemical observations. This new trace element content data, reported here, corroborate our previous results based on the shape, structure, mineralogy, chemical, and isotopic data of the whole meteorite, as well as on a petrographic and chemical composition study of all types of glasses and give strength to a new genetic model that postulates that D'Orbigny (and possibly all angrites) could have formed in the solar nebula under changing redox conditions, more akin to chondritic constituents (e.g., CAIs) than to planetary differentiated rock.Fil: Varela, Maria Eugenia. Universidad Nacional del Sur; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Bahía Blanca; ArgentinaFil: Kurat, Gero. Universidad de Viena; AustriaFil: Zinner, Ernst. University of Washington; Estados UnidosFil: Hoppe, Peter. Institut Max Planck fuer Bioanorganische Chemie; AlemaniaFil: Ntaflos, T.. Universidad de Viena; AustriaFil: Nazarov, M.. Vernadsky Institute; RusiaMeteoritical Soc2005-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/214801Varela, Maria Eugenia; Kurat, Gero; Zinner, Ernst; Hoppe, Peter; Ntaflos, T.; et al.; The non-igneous genesis of angrites: Support from trace element distribution between phases in D’Orbigny; Meteoritical Soc; Meteoritics & Planetary Science; 40; 3; 12-2005; 409-4301086-9379CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://onlinelibrary.wiley.com/doi/abs/10.1111/j.1945-5100.2005.tb00391.xinfo:eu-repo/semantics/altIdentifier/doi/10.1111/j.1945-5100.2005.tb00391.xinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:30:19Zoai:ri.conicet.gov.ar:11336/214801instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-29 10:30:20.052CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
The non-igneous genesis of angrites: Support from trace element distribution between phases in D’Orbigny |
title |
The non-igneous genesis of angrites: Support from trace element distribution between phases in D’Orbigny |
spellingShingle |
The non-igneous genesis of angrites: Support from trace element distribution between phases in D’Orbigny Varela, Maria Eugenia angrites condensacion genesis D´Orbigny |
title_short |
The non-igneous genesis of angrites: Support from trace element distribution between phases in D’Orbigny |
title_full |
The non-igneous genesis of angrites: Support from trace element distribution between phases in D’Orbigny |
title_fullStr |
The non-igneous genesis of angrites: Support from trace element distribution between phases in D’Orbigny |
title_full_unstemmed |
The non-igneous genesis of angrites: Support from trace element distribution between phases in D’Orbigny |
title_sort |
The non-igneous genesis of angrites: Support from trace element distribution between phases in D’Orbigny |
dc.creator.none.fl_str_mv |
Varela, Maria Eugenia Kurat, Gero Zinner, Ernst Hoppe, Peter Ntaflos, T. Nazarov, M. |
author |
Varela, Maria Eugenia |
author_facet |
Varela, Maria Eugenia Kurat, Gero Zinner, Ernst Hoppe, Peter Ntaflos, T. Nazarov, M. |
author_role |
author |
author2 |
Kurat, Gero Zinner, Ernst Hoppe, Peter Ntaflos, T. Nazarov, M. |
author2_role |
author author author author author |
dc.subject.none.fl_str_mv |
angrites condensacion genesis D´Orbigny |
topic |
angrites condensacion genesis D´Orbigny |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.5 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
D'Orbigny is an exceptional angrite. Chemically, it resembles other angrites such as Asuka-881371, Sahara 99555, Lewis Cliff (LEW) 87051, and LEW 86010, but its structure and texture are peculiar. It has a compact and porous lithology, abundant glasses, augite-bearing druses, and chemical and mineralogical properties that are highly unusual for igneous rocks. Our previous studies led us to a new view on angrites: they can possibly be considered as CAIs that grew to larger sizes than the ones we know from carbonaceous chondrites. Thus, angrites may bear a record of rare and special conditions in some part of the early solar nebula. Here we report trace element contents of D'Orbigny phases. Trace element data were obtained from both the porous and the compact part of this meteorite. We have confronted our results with the popular igneous genetic model. According to this model, if all phases of D'Orbigny crystallized from the same system, as an igneous origin implies, a record of this genesis should be expressed in the distribution of trace elements among early and late phases. Our results show that the trace element distribution of the two contemporaneous phases olivine and plagioclase, which form the backbone of the rock, seem to require liquids of different composition. Abundances of highly incompatible elements in all olivines, including the megacrysts, indicate disequilibrium with the bulk rock and suggest liquids very rich in these elements (>10,000 x CI), which is much richer than any fractional crystallization could possibly produce. In addition, trace element contents of late phases are incompatible with formation from the bulk system's residual melt. These results add additional severe constraints to the many conflicts that existed previously between an igneous model for the origin of angrites and the mineralogical and chemical observations. This new trace element content data, reported here, corroborate our previous results based on the shape, structure, mineralogy, chemical, and isotopic data of the whole meteorite, as well as on a petrographic and chemical composition study of all types of glasses and give strength to a new genetic model that postulates that D'Orbigny (and possibly all angrites) could have formed in the solar nebula under changing redox conditions, more akin to chondritic constituents (e.g., CAIs) than to planetary differentiated rock. Fil: Varela, Maria Eugenia. Universidad Nacional del Sur; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Bahía Blanca; Argentina Fil: Kurat, Gero. Universidad de Viena; Austria Fil: Zinner, Ernst. University of Washington; Estados Unidos Fil: Hoppe, Peter. Institut Max Planck fuer Bioanorganische Chemie; Alemania Fil: Ntaflos, T.. Universidad de Viena; Austria Fil: Nazarov, M.. Vernadsky Institute; Rusia |
description |
D'Orbigny is an exceptional angrite. Chemically, it resembles other angrites such as Asuka-881371, Sahara 99555, Lewis Cliff (LEW) 87051, and LEW 86010, but its structure and texture are peculiar. It has a compact and porous lithology, abundant glasses, augite-bearing druses, and chemical and mineralogical properties that are highly unusual for igneous rocks. Our previous studies led us to a new view on angrites: they can possibly be considered as CAIs that grew to larger sizes than the ones we know from carbonaceous chondrites. Thus, angrites may bear a record of rare and special conditions in some part of the early solar nebula. Here we report trace element contents of D'Orbigny phases. Trace element data were obtained from both the porous and the compact part of this meteorite. We have confronted our results with the popular igneous genetic model. According to this model, if all phases of D'Orbigny crystallized from the same system, as an igneous origin implies, a record of this genesis should be expressed in the distribution of trace elements among early and late phases. Our results show that the trace element distribution of the two contemporaneous phases olivine and plagioclase, which form the backbone of the rock, seem to require liquids of different composition. Abundances of highly incompatible elements in all olivines, including the megacrysts, indicate disequilibrium with the bulk rock and suggest liquids very rich in these elements (>10,000 x CI), which is much richer than any fractional crystallization could possibly produce. In addition, trace element contents of late phases are incompatible with formation from the bulk system's residual melt. These results add additional severe constraints to the many conflicts that existed previously between an igneous model for the origin of angrites and the mineralogical and chemical observations. This new trace element content data, reported here, corroborate our previous results based on the shape, structure, mineralogy, chemical, and isotopic data of the whole meteorite, as well as on a petrographic and chemical composition study of all types of glasses and give strength to a new genetic model that postulates that D'Orbigny (and possibly all angrites) could have formed in the solar nebula under changing redox conditions, more akin to chondritic constituents (e.g., CAIs) than to planetary differentiated rock. |
publishDate |
2005 |
dc.date.none.fl_str_mv |
2005-12 |
dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
format |
article |
status_str |
publishedVersion |
dc.identifier.none.fl_str_mv |
http://hdl.handle.net/11336/214801 Varela, Maria Eugenia; Kurat, Gero; Zinner, Ernst; Hoppe, Peter; Ntaflos, T.; et al.; The non-igneous genesis of angrites: Support from trace element distribution between phases in D’Orbigny; Meteoritical Soc; Meteoritics & Planetary Science; 40; 3; 12-2005; 409-430 1086-9379 CONICET Digital CONICET |
url |
http://hdl.handle.net/11336/214801 |
identifier_str_mv |
Varela, Maria Eugenia; Kurat, Gero; Zinner, Ernst; Hoppe, Peter; Ntaflos, T.; et al.; The non-igneous genesis of angrites: Support from trace element distribution between phases in D’Orbigny; Meteoritical Soc; Meteoritics & Planetary Science; 40; 3; 12-2005; 409-430 1086-9379 CONICET Digital CONICET |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/url/https://onlinelibrary.wiley.com/doi/abs/10.1111/j.1945-5100.2005.tb00391.x info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1945-5100.2005.tb00391.x |
dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
eu_rights_str_mv |
openAccess |
rights_invalid_str_mv |
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
dc.format.none.fl_str_mv |
application/pdf application/pdf |
dc.publisher.none.fl_str_mv |
Meteoritical Soc |
publisher.none.fl_str_mv |
Meteoritical Soc |
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reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
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CONICET Digital (CONICET) |
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CONICET Digital (CONICET) |
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Consejo Nacional de Investigaciones Científicas y Técnicas |
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CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas |
repository.mail.fl_str_mv |
dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
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