Amplitude of heat flow variations on Mars from possible shoreline topography

Analyses of the effective elastic thickness of the Martian lithosphere have been previously used to calculate surface heat flow on Mars at different places and times. In this work, I use elevation differences in a putative Late Hesperian shoreline, named Deuteronilus shoreline, and the relation betw...

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Detalhes bibliográficos
Autor: Ruiz Pérez, Javier
Formato: artículo
Fecha de publicación:2003
País:España
Recursos:Universidad Complutense de Madrid (UCM)
Repositorio:Docta Complutense
Idioma:inglés
OAI Identifier:oai:docta.ucm.es:20.500.14352/49327
Acesso em linha:https://hdl.handle.net/20.500.14352/49327
Access Level:acceso abierto
Palavra-chave:550.2
Mars
Heat flow
Deuteronilus shorelines
Martian lithosphere
Geodinámica
2507 Geofísica
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oai_identifier_str oai:docta.ucm.es:20.500.14352/49327
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repository_id_str
spelling Amplitude of heat flow variations on Mars from possible shoreline topographyRuiz Pérez, Javier550.2MarsHeat flowDeuteronilus shorelinesMartian lithosphereGeodinámica2507 GeofísicaAnalyses of the effective elastic thickness of the Martian lithosphere have been previously used to calculate surface heat flow on Mars at different places and times. In this work, I use elevation differences in a putative Late Hesperian shoreline, named Deuteronilus shoreline, and the relation between thermal state and buoyancy of the lithosphere, in order to estimate the amplitude of the variations of surface heat flow on Mars, probably related to the time in which this feature was formed. The results suggest that, if the Deuteronilus shoreline is a true paleo-equipotential surface, the relative amplitude of surface heat flow variations on the shoreline regions in the Late Hesperian were less than present-day ones in terrestrial continental areas. The results are also roughly valid for the outer contact of the Late Hesperian Vastitas Borealis Formation, if this contact is related to the limits of an ancient ocean. These results could imply that large areas of the Martian lithosphere have been tectonothermally stable since at least that time.American Geophysical UnionUniversidad Complutense de Madrid20032003-11-2020032003-11-20journal articlehttp://purl.org/coar/resource_type/c_6501info:eu-repo/semantics/articleapplication/pdfhttps://hdl.handle.net/20.500.14352/49327reponame:Docta Complutenseinstname:Universidad Complutense de Madrid (UCM)Inglésengopen accesshttp://purl.org/coar/access_right/c_abf2info:eu-repo/semantics/openAccessoai:docta.ucm.es:20.500.14352/493272026-06-02T12:44:21Z
dc.title.none.fl_str_mv Amplitude of heat flow variations on Mars from possible shoreline topography
title Amplitude of heat flow variations on Mars from possible shoreline topography
spellingShingle Amplitude of heat flow variations on Mars from possible shoreline topography
Ruiz Pérez, Javier
550.2
Mars
Heat flow
Deuteronilus shorelines
Martian lithosphere
Geodinámica
2507 Geofísica
title_short Amplitude of heat flow variations on Mars from possible shoreline topography
title_full Amplitude of heat flow variations on Mars from possible shoreline topography
title_fullStr Amplitude of heat flow variations on Mars from possible shoreline topography
title_full_unstemmed Amplitude of heat flow variations on Mars from possible shoreline topography
title_sort Amplitude of heat flow variations on Mars from possible shoreline topography
dc.creator.none.fl_str_mv Ruiz Pérez, Javier
author Ruiz Pérez, Javier
author_facet Ruiz Pérez, Javier
author_role author
dc.contributor.none.fl_str_mv Universidad Complutense de Madrid
dc.subject.none.fl_str_mv 550.2
Mars
Heat flow
Deuteronilus shorelines
Martian lithosphere
Geodinámica
2507 Geofísica
topic 550.2
Mars
Heat flow
Deuteronilus shorelines
Martian lithosphere
Geodinámica
2507 Geofísica
description Analyses of the effective elastic thickness of the Martian lithosphere have been previously used to calculate surface heat flow on Mars at different places and times. In this work, I use elevation differences in a putative Late Hesperian shoreline, named Deuteronilus shoreline, and the relation between thermal state and buoyancy of the lithosphere, in order to estimate the amplitude of the variations of surface heat flow on Mars, probably related to the time in which this feature was formed. The results suggest that, if the Deuteronilus shoreline is a true paleo-equipotential surface, the relative amplitude of surface heat flow variations on the shoreline regions in the Late Hesperian were less than present-day ones in terrestrial continental areas. The results are also roughly valid for the outer contact of the Late Hesperian Vastitas Borealis Formation, if this contact is related to the limits of an ancient ocean. These results could imply that large areas of the Martian lithosphere have been tectonothermally stable since at least that time.
publishDate 2003
dc.date.none.fl_str_mv 2003
2003-11-20
2003
2003-11-20
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/20.500.14352/49327
url https://hdl.handle.net/20.500.14352/49327
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 American Geophysical Union
publisher.none.fl_str_mv American Geophysical Union
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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