Oligarchic planetesimal accretion and giant planet formation II
- Autores
- Fortier, Andrea; Brunini, Adrián; Benvenuto, Omar Gustavo
- Año de publicación
- 2009
- Idioma
- español castellano
- Tipo de recurso
- artículo
- Estado
- versión enviada
- Descripción
- Aims. The equation of state calculated by Saumon and collaborators has been adopted in most core-accretion simulations of giant-planet formation performed to date. Since some minor errors have been found in their original paper, we present revised simulations of giant-planet formation that considers a corrected equation of state. \nMethods. We employ the same code as Fortier and collaborators in repeating our previous simulations of the formation of Jupiter. \nResults. Although the general conclusions of Fortier and collaborators remain valid, we obtain significantly lower core masses and shorter formation times in all cases considered. \nConclusions. The minor errors in the previously published equation of state have been shown to affect directly the adiabatic gradient and the specific heat, causing an overestimation of both the core masses and formation times.
- Materia
-
Ciencias Astronómicas
planetología - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- http://creativecommons.org/licenses/by/4.0/
- Repositorio
- Institución
- Comisión de Investigaciones Científicas de la Provincia de Buenos Aires
- OAI Identificador
- oai:digital.cic.gba.gob.ar:11746/3868
Ver los metadatos del registro completo
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CIC Digital (CICBA) |
spelling |
Oligarchic planetesimal accretion and giant planet formation IIFortier, AndreaBrunini, AdriánBenvenuto, Omar GustavoCiencias AstronómicasplanetologíaAims. The equation of state calculated by Saumon and collaborators has been adopted in most core-accretion simulations of giant-planet formation performed to date. Since some minor errors have been found in their original paper, we present revised simulations of giant-planet formation that considers a corrected equation of state. \nMethods. We employ the same code as Fortier and collaborators in repeating our previous simulations of the formation of Jupiter. \nResults. Although the general conclusions of Fortier and collaborators remain valid, we obtain significantly lower core masses and shorter formation times in all cases considered. \nConclusions. The minor errors in the previously published equation of state have been shown to affect directly the adiabatic gradient and the specific heat, causing an overestimation of both the core masses and formation times.2009-01-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/submittedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttps://digital.cic.gba.gob.ar/handle/11746/3868spainfo:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by/4.0/reponame:CIC Digital (CICBA)instname:Comisión de Investigaciones Científicas de la Provincia de Buenos Airesinstacron:CICBA2025-09-29T13:40:00Zoai:digital.cic.gba.gob.ar:11746/3868Institucionalhttp://digital.cic.gba.gob.arOrganismo científico-tecnológicoNo correspondehttp://digital.cic.gba.gob.ar/oai/snrdmarisa.degiusti@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:94412025-09-29 13:40:01.24CIC Digital (CICBA) - Comisión de Investigaciones Científicas de la Provincia de Buenos Airesfalse |
dc.title.none.fl_str_mv |
Oligarchic planetesimal accretion and giant planet formation II |
title |
Oligarchic planetesimal accretion and giant planet formation II |
spellingShingle |
Oligarchic planetesimal accretion and giant planet formation II Fortier, Andrea Ciencias Astronómicas planetología |
title_short |
Oligarchic planetesimal accretion and giant planet formation II |
title_full |
Oligarchic planetesimal accretion and giant planet formation II |
title_fullStr |
Oligarchic planetesimal accretion and giant planet formation II |
title_full_unstemmed |
Oligarchic planetesimal accretion and giant planet formation II |
title_sort |
Oligarchic planetesimal accretion and giant planet formation II |
dc.creator.none.fl_str_mv |
Fortier, Andrea Brunini, Adrián Benvenuto, Omar Gustavo |
author |
Fortier, Andrea |
author_facet |
Fortier, Andrea Brunini, Adrián Benvenuto, Omar Gustavo |
author_role |
author |
author2 |
Brunini, Adrián Benvenuto, Omar Gustavo |
author2_role |
author author |
dc.subject.none.fl_str_mv |
Ciencias Astronómicas planetología |
topic |
Ciencias Astronómicas planetología |
dc.description.none.fl_txt_mv |
Aims. The equation of state calculated by Saumon and collaborators has been adopted in most core-accretion simulations of giant-planet formation performed to date. Since some minor errors have been found in their original paper, we present revised simulations of giant-planet formation that considers a corrected equation of state. \nMethods. We employ the same code as Fortier and collaborators in repeating our previous simulations of the formation of Jupiter. \nResults. Although the general conclusions of Fortier and collaborators remain valid, we obtain significantly lower core masses and shorter formation times in all cases considered. \nConclusions. The minor errors in the previously published equation of state have been shown to affect directly the adiabatic gradient and the specific heat, causing an overestimation of both the core masses and formation times. |
description |
Aims. The equation of state calculated by Saumon and collaborators has been adopted in most core-accretion simulations of giant-planet formation performed to date. Since some minor errors have been found in their original paper, we present revised simulations of giant-planet formation that considers a corrected equation of state. \nMethods. We employ the same code as Fortier and collaborators in repeating our previous simulations of the formation of Jupiter. \nResults. Although the general conclusions of Fortier and collaborators remain valid, we obtain significantly lower core masses and shorter formation times in all cases considered. \nConclusions. The minor errors in the previously published equation of state have been shown to affect directly the adiabatic gradient and the specific heat, causing an overestimation of both the core masses and formation times. |
publishDate |
2009 |
dc.date.none.fl_str_mv |
2009-01-01 |
dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/submittedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
format |
article |
status_str |
submittedVersion |
dc.identifier.none.fl_str_mv |
https://digital.cic.gba.gob.ar/handle/11746/3868 |
url |
https://digital.cic.gba.gob.ar/handle/11746/3868 |
dc.language.none.fl_str_mv |
spa |
language |
spa |
dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/4.0/ |
eu_rights_str_mv |
openAccess |
rights_invalid_str_mv |
http://creativecommons.org/licenses/by/4.0/ |
dc.format.none.fl_str_mv |
application/pdf |
dc.source.none.fl_str_mv |
reponame:CIC Digital (CICBA) instname:Comisión de Investigaciones Científicas de la Provincia de Buenos Aires instacron:CICBA |
reponame_str |
CIC Digital (CICBA) |
collection |
CIC Digital (CICBA) |
instname_str |
Comisión de Investigaciones Científicas de la Provincia de Buenos Aires |
instacron_str |
CICBA |
institution |
CICBA |
repository.name.fl_str_mv |
CIC Digital (CICBA) - Comisión de Investigaciones Científicas de la Provincia de Buenos Aires |
repository.mail.fl_str_mv |
marisa.degiusti@sedici.unlp.edu.ar |
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1844618593482833920 |
score |
13.070432 |