Formation of short-period planets by disc migration
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/stz974 http://hdl.handle.net/11449/188078 |
Resumo: | Protoplanetary discs are thought to be truncated at orbital periods of around 10 d. Therefore, the origin of rocky short-period planets with P < 10 d is a puzzle. We propose that many of these planets may form through the Type-I migration of planets locked into a chain of mutual mean motion resonances. We ran N-body simulations of planetary embryos embedded in a protoplanetary disc. The embryos experienced gravitational scatterings, collisions, disc torques, and dampening of orbital eccentricity and inclination. We then modelled Kepler observations of these planets using a forward model of both the transit probability and the detection efficiency of the Kepler pipeline. We found that planets become locked into long chains of mean motion resonances that migrate in unison. When the chain reaches the edge of the disc, the inner planets are pushed past the edge due to the disc torques acting on the planets farther out in the chain. Our simulated systems successfully reproduce the observed period distribution of short-period Kepler planets between 1 and 2 R⊕. However, we obtain fewer closely packed short-period planets than in the Kepler sample. Our results provide valuable insight into the planet formation process, and suggests that resonance locks, migration, and dynamical instabilities play important roles in the formation and evolution of close-in small exoplanets. |
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Repositório Institucional da UNESP |
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Formation of short-period planets by disc migrationplanets and satellites: dynamical evolution and stabilityplanets and satellites: formationplanets and satellites: generalProtoplanetary discs are thought to be truncated at orbital periods of around 10 d. Therefore, the origin of rocky short-period planets with P < 10 d is a puzzle. We propose that many of these planets may form through the Type-I migration of planets locked into a chain of mutual mean motion resonances. We ran N-body simulations of planetary embryos embedded in a protoplanetary disc. The embryos experienced gravitational scatterings, collisions, disc torques, and dampening of orbital eccentricity and inclination. We then modelled Kepler observations of these planets using a forward model of both the transit probability and the detection efficiency of the Kepler pipeline. We found that planets become locked into long chains of mean motion resonances that migrate in unison. When the chain reaches the edge of the disc, the inner planets are pushed past the edge due to the disc torques acting on the planets farther out in the chain. Our simulated systems successfully reproduce the observed period distribution of short-period Kepler planets between 1 and 2 R⊕. However, we obtain fewer closely packed short-period planets than in the Kepler sample. Our results provide valuable insight into the planet formation process, and suggests that resonance locks, migration, and dynamical instabilities play important roles in the formation and evolution of close-in small exoplanets.Department of Astronomy and Astrophysics 525 Davey Laboratory Pennsylvania State UniversityCenter for Exoplanets and Habitable Worlds 525 Davey Laboratory Pennsylvania State UniversityInstitute for CyberScience Pennsylvania State UniversityUNESP Univ. Estadual Paulista Grupo de Dinâmica Orbital and PlanetologiaUNESP Univ. Estadual Paulista Grupo de Dinâmica Orbital and PlanetologiaPennsylvania State UniversityUniversidade Estadual Paulista (Unesp)Carrera, DanielFord, Eric B.Izidoro, Andre [UNESP]2019-10-06T15:56:36Z2019-10-06T15:56:36Z2019-01-01info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/article3874-3885http://dx.doi.org/10.1093/mnras/stz974Monthly Notices of the Royal Astronomical Society, v. 486, n. 3, p. 3874-3885, 2019.1365-29660035-8711http://hdl.handle.net/11449/18807810.1093/mnras/stz9742-s2.0-85072256219Scopusreponame:Repositório Institucional da UNESPinstname:Universidade Estadual Paulista (UNESP)instacron:UNESPengMonthly Notices of the Royal Astronomical Societyinfo:eu-repo/semantics/openAccess2021-10-22T21:16:13Zoai:repositorio.unesp.br:11449/188078Repositório InstitucionalPUBhttp://repositorio.unesp.br/oai/requestopendoar:29462024-08-05T14:54:03.945547Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP)false |
dc.title.none.fl_str_mv |
Formation of short-period planets by disc migration |
title |
Formation of short-period planets by disc migration |
spellingShingle |
Formation of short-period planets by disc migration Carrera, Daniel planets and satellites: dynamical evolution and stability planets and satellites: formation planets and satellites: general |
title_short |
Formation of short-period planets by disc migration |
title_full |
Formation of short-period planets by disc migration |
title_fullStr |
Formation of short-period planets by disc migration |
title_full_unstemmed |
Formation of short-period planets by disc migration |
title_sort |
Formation of short-period planets by disc migration |
author |
Carrera, Daniel |
author_facet |
Carrera, Daniel Ford, Eric B. Izidoro, Andre [UNESP] |
author_role |
author |
author2 |
Ford, Eric B. Izidoro, Andre [UNESP] |
author2_role |
author author |
dc.contributor.none.fl_str_mv |
Pennsylvania State University Universidade Estadual Paulista (Unesp) |
dc.contributor.author.fl_str_mv |
Carrera, Daniel Ford, Eric B. Izidoro, Andre [UNESP] |
dc.subject.por.fl_str_mv |
planets and satellites: dynamical evolution and stability planets and satellites: formation planets and satellites: general |
topic |
planets and satellites: dynamical evolution and stability planets and satellites: formation planets and satellites: general |
description |
Protoplanetary discs are thought to be truncated at orbital periods of around 10 d. Therefore, the origin of rocky short-period planets with P < 10 d is a puzzle. We propose that many of these planets may form through the Type-I migration of planets locked into a chain of mutual mean motion resonances. We ran N-body simulations of planetary embryos embedded in a protoplanetary disc. The embryos experienced gravitational scatterings, collisions, disc torques, and dampening of orbital eccentricity and inclination. We then modelled Kepler observations of these planets using a forward model of both the transit probability and the detection efficiency of the Kepler pipeline. We found that planets become locked into long chains of mean motion resonances that migrate in unison. When the chain reaches the edge of the disc, the inner planets are pushed past the edge due to the disc torques acting on the planets farther out in the chain. Our simulated systems successfully reproduce the observed period distribution of short-period Kepler planets between 1 and 2 R⊕. However, we obtain fewer closely packed short-period planets than in the Kepler sample. Our results provide valuable insight into the planet formation process, and suggests that resonance locks, migration, and dynamical instabilities play important roles in the formation and evolution of close-in small exoplanets. |
publishDate |
2019 |
dc.date.none.fl_str_mv |
2019-10-06T15:56:36Z 2019-10-06T15:56:36Z 2019-01-01 |
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/stz974 Monthly Notices of the Royal Astronomical Society, v. 486, n. 3, p. 3874-3885, 2019. 1365-2966 0035-8711 http://hdl.handle.net/11449/188078 10.1093/mnras/stz974 2-s2.0-85072256219 |
url |
http://dx.doi.org/10.1093/mnras/stz974 http://hdl.handle.net/11449/188078 |
identifier_str_mv |
Monthly Notices of the Royal Astronomical Society, v. 486, n. 3, p. 3874-3885, 2019. 1365-2966 0035-8711 10.1093/mnras/stz974 2-s2.0-85072256219 |
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 |
3874-3885 |
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_ |
1808128433526407168 |