Adapting a solid accretion scenario for migrating planets in FARGO3D
Autor(a) principal: | |
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Data de Publicação: | 2019 |
Outros Autores: | , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UNESP |
Texto Completo: | http://dx.doi.org/10.1093/mnras/stz2762 http://hdl.handle.net/11449/198545 |
Resumo: | In this work, we adapt a module for planetary formation within the hydrodynamic code FARGO3D. Planetary formation is modelled by a solid core accretion scenario, with the core growing in oligarchic regime. The initial superficial density of planetesimals is proportional to the initial superficial density of gas in the disc. We include a numerical approach to describe the evolution of the eccentricity and the inclination of planetesimals during the formation. This approach impacts directly on the accretion rate of solids. When the core reaches a critical mass, gas accretion begins, following the original FARGO scheme adapted to the FARGO3D code. To exemplify how the module for planetary formation can be used, we investigate the migration of a planet in a 2D, locally isothermal gas disc with a prescribed accretion rate, analysing the time-scale involved in the planetary migration process along with the time-scale for planetary formation. The analysis reveals that the mass of the nucleus must be close to its critical value when crossing the ice line to avoid the planet's fall into the stellar envelope. This will allow enough time for the planet to initiate runaway gas accretion, leading to a rapid mass increase and entering type II planetary migration. |
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Repositório Institucional da UNESP |
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Adapting a solid accretion scenario for migrating planets in FARGO3DPlanet-star interactionsPlanets and satellites: formationProtoplanetary discsIn this work, we adapt a module for planetary formation within the hydrodynamic code FARGO3D. Planetary formation is modelled by a solid core accretion scenario, with the core growing in oligarchic regime. The initial superficial density of planetesimals is proportional to the initial superficial density of gas in the disc. We include a numerical approach to describe the evolution of the eccentricity and the inclination of planetesimals during the formation. This approach impacts directly on the accretion rate of solids. When the core reaches a critical mass, gas accretion begins, following the original FARGO scheme adapted to the FARGO3D code. To exemplify how the module for planetary formation can be used, we investigate the migration of a planet in a 2D, locally isothermal gas disc with a prescribed accretion rate, analysing the time-scale involved in the planetary migration process along with the time-scale for planetary formation. The analysis reveals that the mass of the nucleus must be close to its critical value when crossing the ice line to avoid the planet's fall into the stellar envelope. This will allow enough time for the planet to initiate runaway gas accretion, leading to a rapid mass increase and entering type II planetary migration.Instituto Astronômico Geofísico e Ciência Atmosféricas Universidade de São Paulo, Rua do Matão 1226São Paulo State University - UNESP, Av. Profa. Isette Corrêa Fontão, 505São Paulo State University - UNESP, Av. Profa. Isette Corrêa Fontão, 505Universidade de São Paulo (USP)Universidade Estadual Paulista (Unesp)DePaula, L. A.Michtchenko, T. A.Sousa-Silva, P. A. [UNESP]2020-12-12T01:15:49Z2020-12-12T01:15:49Z2019-12-01info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/article2336-2346http://dx.doi.org/10.1093/mnras/stz2762Monthly Notices of the Royal Astronomical Society, v. 490, n. 2, p. 2336-2346, 2019.1365-29660035-8711http://hdl.handle.net/11449/19854510.1093/mnras/stz27622-s2.0-85079681599Scopusreponame:Repositório Institucional da UNESPinstname:Universidade Estadual Paulista (UNESP)instacron:UNESPengMonthly Notices of the Royal Astronomical Societyinfo:eu-repo/semantics/openAccess2021-10-22T14:03:08Zoai:repositorio.unesp.br:11449/198545Repositório InstitucionalPUBhttp://repositorio.unesp.br/oai/requestopendoar:29462024-08-05T21:47:30.613555Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP)false |
dc.title.none.fl_str_mv |
Adapting a solid accretion scenario for migrating planets in FARGO3D |
title |
Adapting a solid accretion scenario for migrating planets in FARGO3D |
spellingShingle |
Adapting a solid accretion scenario for migrating planets in FARGO3D DePaula, L. A. Planet-star interactions Planets and satellites: formation Protoplanetary discs |
title_short |
Adapting a solid accretion scenario for migrating planets in FARGO3D |
title_full |
Adapting a solid accretion scenario for migrating planets in FARGO3D |
title_fullStr |
Adapting a solid accretion scenario for migrating planets in FARGO3D |
title_full_unstemmed |
Adapting a solid accretion scenario for migrating planets in FARGO3D |
title_sort |
Adapting a solid accretion scenario for migrating planets in FARGO3D |
author |
DePaula, L. A. |
author_facet |
DePaula, L. A. Michtchenko, T. A. Sousa-Silva, P. A. [UNESP] |
author_role |
author |
author2 |
Michtchenko, T. A. Sousa-Silva, P. A. [UNESP] |
author2_role |
author author |
dc.contributor.none.fl_str_mv |
Universidade de São Paulo (USP) Universidade Estadual Paulista (Unesp) |
dc.contributor.author.fl_str_mv |
DePaula, L. A. Michtchenko, T. A. Sousa-Silva, P. A. [UNESP] |
dc.subject.por.fl_str_mv |
Planet-star interactions Planets and satellites: formation Protoplanetary discs |
topic |
Planet-star interactions Planets and satellites: formation Protoplanetary discs |
description |
In this work, we adapt a module for planetary formation within the hydrodynamic code FARGO3D. Planetary formation is modelled by a solid core accretion scenario, with the core growing in oligarchic regime. The initial superficial density of planetesimals is proportional to the initial superficial density of gas in the disc. We include a numerical approach to describe the evolution of the eccentricity and the inclination of planetesimals during the formation. This approach impacts directly on the accretion rate of solids. When the core reaches a critical mass, gas accretion begins, following the original FARGO scheme adapted to the FARGO3D code. To exemplify how the module for planetary formation can be used, we investigate the migration of a planet in a 2D, locally isothermal gas disc with a prescribed accretion rate, analysing the time-scale involved in the planetary migration process along with the time-scale for planetary formation. The analysis reveals that the mass of the nucleus must be close to its critical value when crossing the ice line to avoid the planet's fall into the stellar envelope. This will allow enough time for the planet to initiate runaway gas accretion, leading to a rapid mass increase and entering type II planetary migration. |
publishDate |
2019 |
dc.date.none.fl_str_mv |
2019-12-01 2020-12-12T01:15:49Z 2020-12-12T01:15:49Z |
dc.type.status.fl_str_mv |
info:eu-repo/semantics/publishedVersion |
dc.type.driver.fl_str_mv |
info:eu-repo/semantics/article |
format |
article |
status_str |
publishedVersion |
dc.identifier.uri.fl_str_mv |
http://dx.doi.org/10.1093/mnras/stz2762 Monthly Notices of the Royal Astronomical Society, v. 490, n. 2, p. 2336-2346, 2019. 1365-2966 0035-8711 http://hdl.handle.net/11449/198545 10.1093/mnras/stz2762 2-s2.0-85079681599 |
url |
http://dx.doi.org/10.1093/mnras/stz2762 http://hdl.handle.net/11449/198545 |
identifier_str_mv |
Monthly Notices of the Royal Astronomical Society, v. 490, n. 2, p. 2336-2346, 2019. 1365-2966 0035-8711 10.1093/mnras/stz2762 2-s2.0-85079681599 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
Monthly Notices of the Royal Astronomical Society |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
dc.format.none.fl_str_mv |
2336-2346 |
dc.source.none.fl_str_mv |
Scopus reponame:Repositório Institucional da UNESP instname:Universidade Estadual Paulista (UNESP) instacron:UNESP |
instname_str |
Universidade Estadual Paulista (UNESP) |
instacron_str |
UNESP |
institution |
UNESP |
reponame_str |
Repositório Institucional da UNESP |
collection |
Repositório Institucional da UNESP |
repository.name.fl_str_mv |
Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP) |
repository.mail.fl_str_mv |
|
_version_ |
1808129358542405632 |