Oligarchic planetesimal accretion and giant planet formation
- Autores
- Fortier, Andrea; Benvenuto, Omar Gustavo; Brunini, Adrian
- Año de publicación
- 2007
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Aims. In the context of the core instability model, we present calculations of in situ giant planet formation. The oligarchic growth regime of solid protoplanets is the model adopted for the growth of the core. This growth regime for the core has not been considered before in full evolutionary calculations of this kind. Methods. The full differential equations of giant planet formation were numerically solved with an adaptation of a Henyey-type code. The planetesimals accretion rate was coupled in a self-consistent way to the envelope’s evolution. Results. We performed several simulations for the formation of a Jupiter-like object by assuming various surface densities for the protoplanetary disc and two different sizes for the accreted planetesimals. We first focus our study on the atmospheric gas drag that the incoming planetesimals suffer. We find that this effect gives rise to a major enhancement on the effective capture radius of the protoplanet, thus leading to an average timescale reduction of ∼30%–55% and ultimately to an increase by a factor of 2 of the final mass of solids accreted as compared to the situation in which drag effects are neglected. In addition, we also examine the importance of the size of accreted planetesimals on the whole formation process. With regard to this second point, we find that for a swarm of planetesimals having a radius of 10 km, the formation time is a factor 2 to 3 shorter than that of planetesimals of 100 km, the factor depending on the surface density of the nebula. Moreover, planetesimal size does not seem to have a significant impact on the final mass of the core.
Fil: Fortier, Andrea. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Benvenuto, Omar Gustavo. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Brunini, Adrian. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina - Materia
-
Solar System
Giant planets
Origins of planets
Numerical methods
Satellites
Planets - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/42103
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oai:ri.conicet.gov.ar:11336/42103 |
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spelling |
Oligarchic planetesimal accretion and giant planet formationFortier, AndreaBenvenuto, Omar GustavoBrunini, AdrianSolar SystemGiant planetsOrigins of planetsNumerical methodsSatellitesPlanetshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Aims. In the context of the core instability model, we present calculations of in situ giant planet formation. The oligarchic growth regime of solid protoplanets is the model adopted for the growth of the core. This growth regime for the core has not been considered before in full evolutionary calculations of this kind. Methods. The full differential equations of giant planet formation were numerically solved with an adaptation of a Henyey-type code. The planetesimals accretion rate was coupled in a self-consistent way to the envelope’s evolution. Results. We performed several simulations for the formation of a Jupiter-like object by assuming various surface densities for the protoplanetary disc and two different sizes for the accreted planetesimals. We first focus our study on the atmospheric gas drag that the incoming planetesimals suffer. We find that this effect gives rise to a major enhancement on the effective capture radius of the protoplanet, thus leading to an average timescale reduction of ∼30%–55% and ultimately to an increase by a factor of 2 of the final mass of solids accreted as compared to the situation in which drag effects are neglected. In addition, we also examine the importance of the size of accreted planetesimals on the whole formation process. With regard to this second point, we find that for a swarm of planetesimals having a radius of 10 km, the formation time is a factor 2 to 3 shorter than that of planetesimals of 100 km, the factor depending on the surface density of the nebula. Moreover, planetesimal size does not seem to have a significant impact on the final mass of the core.Fil: Fortier, Andrea. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Benvenuto, Omar Gustavo. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Brunini, Adrian. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaEDP Sciences2007-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/42103Fortier, Andrea; Benvenuto, Omar Gustavo; Brunini, Adrian; Oligarchic planetesimal accretion and giant planet formation; EDP Sciences; Astronomy and Astrophysics; 473; 1; 12-2007; 311-3220004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20066729info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2007/37/aa6729-06/aa6729-06.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:45:38Zoai:ri.conicet.gov.ar:11336/42103instacron: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 09:45:39.053CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
Oligarchic planetesimal accretion and giant planet formation |
title |
Oligarchic planetesimal accretion and giant planet formation |
spellingShingle |
Oligarchic planetesimal accretion and giant planet formation Fortier, Andrea Solar System Giant planets Origins of planets Numerical methods Satellites Planets |
title_short |
Oligarchic planetesimal accretion and giant planet formation |
title_full |
Oligarchic planetesimal accretion and giant planet formation |
title_fullStr |
Oligarchic planetesimal accretion and giant planet formation |
title_full_unstemmed |
Oligarchic planetesimal accretion and giant planet formation |
title_sort |
Oligarchic planetesimal accretion and giant planet formation |
dc.creator.none.fl_str_mv |
Fortier, Andrea Benvenuto, Omar Gustavo Brunini, Adrian |
author |
Fortier, Andrea |
author_facet |
Fortier, Andrea Benvenuto, Omar Gustavo Brunini, Adrian |
author_role |
author |
author2 |
Benvenuto, Omar Gustavo Brunini, Adrian |
author2_role |
author author |
dc.subject.none.fl_str_mv |
Solar System Giant planets Origins of planets Numerical methods Satellites Planets |
topic |
Solar System Giant planets Origins of planets Numerical methods Satellites Planets |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
Aims. In the context of the core instability model, we present calculations of in situ giant planet formation. The oligarchic growth regime of solid protoplanets is the model adopted for the growth of the core. This growth regime for the core has not been considered before in full evolutionary calculations of this kind. Methods. The full differential equations of giant planet formation were numerically solved with an adaptation of a Henyey-type code. The planetesimals accretion rate was coupled in a self-consistent way to the envelope’s evolution. Results. We performed several simulations for the formation of a Jupiter-like object by assuming various surface densities for the protoplanetary disc and two different sizes for the accreted planetesimals. We first focus our study on the atmospheric gas drag that the incoming planetesimals suffer. We find that this effect gives rise to a major enhancement on the effective capture radius of the protoplanet, thus leading to an average timescale reduction of ∼30%–55% and ultimately to an increase by a factor of 2 of the final mass of solids accreted as compared to the situation in which drag effects are neglected. In addition, we also examine the importance of the size of accreted planetesimals on the whole formation process. With regard to this second point, we find that for a swarm of planetesimals having a radius of 10 km, the formation time is a factor 2 to 3 shorter than that of planetesimals of 100 km, the factor depending on the surface density of the nebula. Moreover, planetesimal size does not seem to have a significant impact on the final mass of the core. Fil: Fortier, Andrea. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina Fil: Benvenuto, Omar Gustavo. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina Fil: Brunini, Adrian. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina |
description |
Aims. In the context of the core instability model, we present calculations of in situ giant planet formation. The oligarchic growth regime of solid protoplanets is the model adopted for the growth of the core. This growth regime for the core has not been considered before in full evolutionary calculations of this kind. Methods. The full differential equations of giant planet formation were numerically solved with an adaptation of a Henyey-type code. The planetesimals accretion rate was coupled in a self-consistent way to the envelope’s evolution. Results. We performed several simulations for the formation of a Jupiter-like object by assuming various surface densities for the protoplanetary disc and two different sizes for the accreted planetesimals. We first focus our study on the atmospheric gas drag that the incoming planetesimals suffer. We find that this effect gives rise to a major enhancement on the effective capture radius of the protoplanet, thus leading to an average timescale reduction of ∼30%–55% and ultimately to an increase by a factor of 2 of the final mass of solids accreted as compared to the situation in which drag effects are neglected. In addition, we also examine the importance of the size of accreted planetesimals on the whole formation process. With regard to this second point, we find that for a swarm of planetesimals having a radius of 10 km, the formation time is a factor 2 to 3 shorter than that of planetesimals of 100 km, the factor depending on the surface density of the nebula. Moreover, planetesimal size does not seem to have a significant impact on the final mass of the core. |
publishDate |
2007 |
dc.date.none.fl_str_mv |
2007-12 |
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/11336/42103 Fortier, Andrea; Benvenuto, Omar Gustavo; Brunini, Adrian; Oligarchic planetesimal accretion and giant planet formation; EDP Sciences; Astronomy and Astrophysics; 473; 1; 12-2007; 311-322 0004-6361 CONICET Digital CONICET |
url |
http://hdl.handle.net/11336/42103 |
identifier_str_mv |
Fortier, Andrea; Benvenuto, Omar Gustavo; Brunini, Adrian; Oligarchic planetesimal accretion and giant planet formation; EDP Sciences; Astronomy and Astrophysics; 473; 1; 12-2007; 311-322 0004-6361 CONICET Digital CONICET |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20066729 info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2007/37/aa6729-06/aa6729-06.html |
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 application/pdf |
dc.publisher.none.fl_str_mv |
EDP Sciences |
publisher.none.fl_str_mv |
EDP Sciences |
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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1844613429366620160 |
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13.070432 |