Adapting a solid accretion scenario for migrating planets in FARGO3D

Detalhes bibliográficos
Autor(a) principal: DePaula, L. A.
Data de Publicação: 2019
Outros Autores: Michtchenko, T. A., Sousa-Silva, P. A. [UNESP]
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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spelling 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
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