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
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/214801

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network_name_str CONICET Digital (CONICET)
spelling 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
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv 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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