Chasma Australe, Mars: Structural Framework for a Catastrophic Outflow Origin

Chasma Australe, 500 km long and up to 80 km wide, is the most remarkable of the martian south pole erosional reentrants carved in the polar layered deposits. We have interpreted Chasma Australe erosional and depositional features as evidence for a flood origin, which we have reconstructed using a m...

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Autores: Anguita Virella, Francisco, Babín Vich, Rosa Blanca, Benito, Gerardo, Gómez Ortiz, David, Collado, Ana, Rice, James W.
Tipo de recurso: artículo
Fecha de publicación:2000
País:España
Institución:Universidad Complutense de Madrid (UCM)
Repositorio:Docta Complutense
Idioma:inglés
OAI Identifier:oai:docta.ucm.es:20.500.14352/59059
Acceso en línea:https://hdl.handle.net/20.500.14352/59059
Access Level:acceso abierto
Palabra clave:550.2
Chasma Australe
Mars
Geología
2506 Geología
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spelling Chasma Australe, Mars: Structural Framework for a Catastrophic Outflow OriginAnguita Virella, FranciscoBabín Vich, Rosa BlancaBenito, GerardoGómez Ortiz, DavidCollado, AnaRice, James W.550.2Chasma AustraleMarsGeología2506 GeologíaChasma Australe, 500 km long and up to 80 km wide, is the most remarkable of the martian south pole erosional reentrants carved in the polar layered deposits. We have interpreted Chasma Australe erosional and depositional features as evidence for a flood origin, which we have reconstructed using a modified Manning equation. The main characteristics of the flow are a water velocity between 30 and 50 m s¡1 and discharge values between 7 x 10^8 and 3 x 10^9 m3 s-1, very near to MGS data-based estimations for martian outflow channels (D. E. Smith et al. 1998, Science 279, 1686–1692). We thus postulate that Chasma Australe originated in a catastrophic flood. The tectonic study of an area (roughly 20 million km2 in size) around Mars’ south pole included the measurement and projection in rose diagrams of more than 300 lineaments, of which 85 were wrinkle ridges and the rest straight scarps. The whole set of lineaments can be explained by a stress field with a d1 N10ºE in strike, the wrinkle ridges being reverse faults and the other lineaments direct and strike-slip faults. The straight layout of parts of Chasma Australe almost 200 km long suggests that the chasma was carved following a fracture network. The effectiveness of the erosional process (the canyon is up to 1000 m deep) leads us to suspect that this carving was preceded by a sapping period. Endogenetic and exogenetic processes would thus have contributed to the origin of this landformElsevier Science B.V., AmsterdamUniversidad Complutense de Madrid20002000-01-0120002000-01-01journal articlehttp://purl.org/coar/resource_type/c_6501info:eu-repo/semantics/articleapplication/pdfhttps://hdl.handle.net/20.500.14352/59059reponame:Docta Complutenseinstname:Universidad Complutense de Madrid (UCM)Inglésengopen accesshttp://purl.org/coar/access_right/c_abf2info:eu-repo/semantics/openAccessoai:docta.ucm.es:20.500.14352/590592026-06-02T12:44:21Z
dc.title.none.fl_str_mv Chasma Australe, Mars: Structural Framework for a Catastrophic Outflow Origin
title Chasma Australe, Mars: Structural Framework for a Catastrophic Outflow Origin
spellingShingle Chasma Australe, Mars: Structural Framework for a Catastrophic Outflow Origin
Anguita Virella, Francisco
550.2
Chasma Australe
Mars
Geología
2506 Geología
title_short Chasma Australe, Mars: Structural Framework for a Catastrophic Outflow Origin
title_full Chasma Australe, Mars: Structural Framework for a Catastrophic Outflow Origin
title_fullStr Chasma Australe, Mars: Structural Framework for a Catastrophic Outflow Origin
title_full_unstemmed Chasma Australe, Mars: Structural Framework for a Catastrophic Outflow Origin
title_sort Chasma Australe, Mars: Structural Framework for a Catastrophic Outflow Origin
dc.creator.none.fl_str_mv Anguita Virella, Francisco
Babín Vich, Rosa Blanca
Benito, Gerardo
Gómez Ortiz, David
Collado, Ana
Rice, James W.
author Anguita Virella, Francisco
author_facet Anguita Virella, Francisco
Babín Vich, Rosa Blanca
Benito, Gerardo
Gómez Ortiz, David
Collado, Ana
Rice, James W.
author_role author
author2 Babín Vich, Rosa Blanca
Benito, Gerardo
Gómez Ortiz, David
Collado, Ana
Rice, James W.
author2_role author
author
author
author
author
dc.contributor.none.fl_str_mv Universidad Complutense de Madrid
dc.subject.none.fl_str_mv 550.2
Chasma Australe
Mars
Geología
2506 Geología
topic 550.2
Chasma Australe
Mars
Geología
2506 Geología
description Chasma Australe, 500 km long and up to 80 km wide, is the most remarkable of the martian south pole erosional reentrants carved in the polar layered deposits. We have interpreted Chasma Australe erosional and depositional features as evidence for a flood origin, which we have reconstructed using a modified Manning equation. The main characteristics of the flow are a water velocity between 30 and 50 m s¡1 and discharge values between 7 x 10^8 and 3 x 10^9 m3 s-1, very near to MGS data-based estimations for martian outflow channels (D. E. Smith et al. 1998, Science 279, 1686–1692). We thus postulate that Chasma Australe originated in a catastrophic flood. The tectonic study of an area (roughly 20 million km2 in size) around Mars’ south pole included the measurement and projection in rose diagrams of more than 300 lineaments, of which 85 were wrinkle ridges and the rest straight scarps. The whole set of lineaments can be explained by a stress field with a d1 N10ºE in strike, the wrinkle ridges being reverse faults and the other lineaments direct and strike-slip faults. The straight layout of parts of Chasma Australe almost 200 km long suggests that the chasma was carved following a fracture network. The effectiveness of the erosional process (the canyon is up to 1000 m deep) leads us to suspect that this carving was preceded by a sapping period. Endogenetic and exogenetic processes would thus have contributed to the origin of this landform
publishDate 2000
dc.date.none.fl_str_mv 2000
2000-01-01
2000
2000-01-01
dc.type.none.fl_str_mv journal article
http://purl.org/coar/resource_type/c_6501
dc.type.openaire.fl_str_mv info:eu-repo/semantics/article
format article
dc.identifier.none.fl_str_mv https://hdl.handle.net/20.500.14352/59059
url https://hdl.handle.net/20.500.14352/59059
dc.language.none.fl_str_mv Inglés
eng
language_invalid_str_mv Inglés
language eng
dc.rights.none.fl_str_mv open access
http://purl.org/coar/access_right/c_abf2
dc.rights.openaire.fl_str_mv info:eu-repo/semantics/openAccess
rights_invalid_str_mv open access
http://purl.org/coar/access_right/c_abf2
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv Elsevier Science B.V., Amsterdam
publisher.none.fl_str_mv Elsevier Science B.V., Amsterdam
dc.source.none.fl_str_mv reponame:Docta Complutense
instname:Universidad Complutense de Madrid (UCM)
instname_str Universidad Complutense de Madrid (UCM)
reponame_str Docta Complutense
collection Docta Complutense
repository.name.fl_str_mv
repository.mail.fl_str_mv
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score 15.301603

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