Should paleoshorelines of ancient martian oceans be close to present-day equipotential surfaces?

Thermal isostasy provides a link between surface elevation and thermal state of the lithosphere. Variations in martian surface heat flow, similar to those observed in terrestrial continental tectonothermally stable areas, could result in elevation differences of kilometric scale through differential...

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Detalhes bibliográficos
Autores: Ruiz Pérez, Javier, Fairén, Alberto G., Dohm, James M., Tejero López, Rosa, Castilla Cañamero, Gabriel, Álvarez Gómez, José Antonio, Uceda, Esther R.
Tipo de documento: artigo
Data de publicação:2004
País:España
Recursos:Universidad Complutense de Madrid (UCM)
Repositório:Docta Complutense
Idioma:inglês
OAI Identifier:oai:docta.ucm.es:20.500.14352/51576
Acesso em linha:https://hdl.handle.net/20.500.14352/51576
Access Level:Acceso aberto
Palavra-chave:550.2
Martian oceans
Geodinámica
2507 Geofísica
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oai_identifier_str oai:docta.ucm.es:20.500.14352/51576
network_acronym_str ES
network_name_str España
repository_id_str
spelling Should paleoshorelines of ancient martian oceans be close to present-day equipotential surfaces?Ruiz Pérez, JavierFairén, Alberto G.Dohm, James M.Tejero López, RosaCastilla Cañamero, GabrielÁlvarez Gómez, José AntonioUceda, Esther R.550.2Martian oceansGeodinámica2507 GeofísicaThermal isostasy provides a link between surface elevation and thermal state of the lithosphere. Variations in martian surface heat flow, similar to those observed in terrestrial continental tectonothermally stable areas, could result in elevation differences of kilometric scale through differential thermal isostasy. This effect is enhanced with the increase of heat sources located within the crust. Local differences in the thermal history of the Mars’ lithosphere could have appreciably distorted the original long-avelength topography of putative martian paleoshorelines. This work hows that a paleoequipotential surface does not necessarily have to fit well a present-day equipotential surface, and that diverse processes, including thermal isostasy and operating throughout the martian history, must be taken into account when evaluating paleoshorelines through assessment of high-resolution topography.ESA Publications Division.Universidad Complutense de Madrid20042004-01-0120042004-01-01journal articlehttp://purl.org/coar/resource_type/c_6501info:eu-repo/semantics/articleapplication/pdfhttps://hdl.handle.net/20.500.14352/51576reponame:Docta Complutenseinstname:Universidad Complutense de Madrid (UCM)Inglésengopen accesshttp://purl.org/coar/access_right/c_abf2info:eu-repo/semantics/openAccessoai:docta.ucm.es:20.500.14352/515762026-06-02T12:44:21Z
dc.title.none.fl_str_mv Should paleoshorelines of ancient martian oceans be close to present-day equipotential surfaces?
title Should paleoshorelines of ancient martian oceans be close to present-day equipotential surfaces?
spellingShingle Should paleoshorelines of ancient martian oceans be close to present-day equipotential surfaces?
Ruiz Pérez, Javier
550.2
Martian oceans
Geodinámica
2507 Geofísica
title_short Should paleoshorelines of ancient martian oceans be close to present-day equipotential surfaces?
title_full Should paleoshorelines of ancient martian oceans be close to present-day equipotential surfaces?
title_fullStr Should paleoshorelines of ancient martian oceans be close to present-day equipotential surfaces?
title_full_unstemmed Should paleoshorelines of ancient martian oceans be close to present-day equipotential surfaces?
title_sort Should paleoshorelines of ancient martian oceans be close to present-day equipotential surfaces?
dc.creator.none.fl_str_mv Ruiz Pérez, Javier
Fairén, Alberto G.
Dohm, James M.
Tejero López, Rosa
Castilla Cañamero, Gabriel
Álvarez Gómez, José Antonio
Uceda, Esther R.
author Ruiz Pérez, Javier
author_facet Ruiz Pérez, Javier
Fairén, Alberto G.
Dohm, James M.
Tejero López, Rosa
Castilla Cañamero, Gabriel
Álvarez Gómez, José Antonio
Uceda, Esther R.
author_role author
author2 Fairén, Alberto G.
Dohm, James M.
Tejero López, Rosa
Castilla Cañamero, Gabriel
Álvarez Gómez, José Antonio
Uceda, Esther R.
author2_role author
author
author
author
author
author
dc.contributor.none.fl_str_mv Universidad Complutense de Madrid
dc.subject.none.fl_str_mv 550.2
Martian oceans
Geodinámica
2507 Geofísica
topic 550.2
Martian oceans
Geodinámica
2507 Geofísica
description Thermal isostasy provides a link between surface elevation and thermal state of the lithosphere. Variations in martian surface heat flow, similar to those observed in terrestrial continental tectonothermally stable areas, could result in elevation differences of kilometric scale through differential thermal isostasy. This effect is enhanced with the increase of heat sources located within the crust. Local differences in the thermal history of the Mars’ lithosphere could have appreciably distorted the original long-avelength topography of putative martian paleoshorelines. This work hows that a paleoequipotential surface does not necessarily have to fit well a present-day equipotential surface, and that diverse processes, including thermal isostasy and operating throughout the martian history, must be taken into account when evaluating paleoshorelines through assessment of high-resolution topography.
publishDate 2004
dc.date.none.fl_str_mv 2004
2004-01-01
2004
2004-01-01
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/20.500.14352/51576
url https://hdl.handle.net/20.500.14352/51576
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 ESA Publications Division.
publisher.none.fl_str_mv ESA Publications Division.
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
_version_ 1869422870523805696
score 15,301629

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