The origins of nearly coplanar, non-resonant systems of close-in super-Earths
Autor(a) principal: | |
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Data de Publicação: | 2020 |
Outros Autores: | , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UNESP |
Texto Completo: | http://dx.doi.org/10.1093/mnras/staa2112 http://hdl.handle.net/11449/205432 |
Resumo: | Some systems of close-in 'super-Earths' contain five or more planets on non-resonant but compact and nearly coplanar orbits. The Kepler-11 system is an iconic representative of this class of system. It is challenging to explain their origins given that planet-disc interactions are thought to be essential to maintain such a high degree of coplanarity, yet these same interactions invariably cause planets to migrate into chains of mean motion resonances. Here, we mine a large data set of dynamical simulations of super-Earth formation by migration. These simulations match the observed period ratio distribution as long as the vast majority of planet pairs in resonance become dynamically unstable. When instabilities take place resonances are broken during a late phase of giant impacts, and typical surviving systems have planet pairs with significant mutual orbital inclinations. However, a subset of our unstable simulations matches the Kepler-11 system in terms of coplanarity, compactness, planet-multiplicity, and non-resonant state. This subset has dynamical instability phases typically much shorter than ordinary systems. Unstable systems may keep a high degree of coplanarity post-instability if planets collide at very low orbital inclinations (<1°) or if collisions promote efficient damping of orbital inclinations. If planetary scattering during the instability takes place at low orbital inclinations (i < 1°), orbital inclinations are barely increased by encounters before planets collide. When planetary scattering pumps orbital inclinations to higher values (>1°) planets tend to collide at higher mutual orbital inclinations, but depending on the geometry of collisions mergers' orbital inclinations may be efficiently damped. Each of these formation pathways can produce analogues to the Kepler-11 system. |
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The origins of nearly coplanar, non-resonant systems of close-in super-EarthsPlanets and satellites: formationProtoplanetary discsSome systems of close-in 'super-Earths' contain five or more planets on non-resonant but compact and nearly coplanar orbits. The Kepler-11 system is an iconic representative of this class of system. It is challenging to explain their origins given that planet-disc interactions are thought to be essential to maintain such a high degree of coplanarity, yet these same interactions invariably cause planets to migrate into chains of mean motion resonances. Here, we mine a large data set of dynamical simulations of super-Earth formation by migration. These simulations match the observed period ratio distribution as long as the vast majority of planet pairs in resonance become dynamically unstable. When instabilities take place resonances are broken during a late phase of giant impacts, and typical surviving systems have planet pairs with significant mutual orbital inclinations. However, a subset of our unstable simulations matches the Kepler-11 system in terms of coplanarity, compactness, planet-multiplicity, and non-resonant state. This subset has dynamical instability phases typically much shorter than ordinary systems. Unstable systems may keep a high degree of coplanarity post-instability if planets collide at very low orbital inclinations (<1°) or if collisions promote efficient damping of orbital inclinations. If planetary scattering during the instability takes place at low orbital inclinations (i < 1°), orbital inclinations are barely increased by encounters before planets collide. When planetary scattering pumps orbital inclinations to higher values (>1°) planets tend to collide at higher mutual orbital inclinations, but depending on the geometry of collisions mergers' orbital inclinations may be efficiently damped. Each of these formation pathways can produce analogues to the Kepler-11 system.Unesp Universidade Estadual Paulista Grupo de Dinâmica Orbital e PlanetologiaDepartment of Earth Environmental and Planetary Sciences Ms 126 Rice UniversityLaboratoire d'Astrophysique de Bordeaux Univ. Bordeaux Cnrs, B18N, allée Geoffroy Saint-HilaireMax-Planck-Institut für Astronomie, Konigstuhl 17Unesp Universidade Estadual Paulista Grupo de Dinâmica Orbital e PlanetologiaUniversidade Estadual Paulista (Unesp)Rice UniversityCnrsMax-Planck-Institut für AstronomieEsteves, Leandro [UNESP]Izidoro, André [UNESP]Raymond, Sean N.Bitsch, Bertram2021-06-25T10:15:12Z2021-06-25T10:15:12Z2020-09-01info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/article2493-2500http://dx.doi.org/10.1093/mnras/staa2112Monthly Notices of the Royal Astronomical Society, v. 497, n. 2, p. 2493-2500, 2020.1365-29660035-8711http://hdl.handle.net/11449/20543210.1093/mnras/staa21122-s2.0-85095444023Scopusreponame:Repositório Institucional da UNESPinstname:Universidade Estadual Paulista (UNESP)instacron:UNESPengMonthly Notices of the Royal Astronomical Societyinfo:eu-repo/semantics/openAccess2021-10-23T14:26:44Zoai:repositorio.unesp.br:11449/205432Repositório InstitucionalPUBhttp://repositorio.unesp.br/oai/requestopendoar:29462024-08-05T22:29:01.184904Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP)false |
dc.title.none.fl_str_mv |
The origins of nearly coplanar, non-resonant systems of close-in super-Earths |
title |
The origins of nearly coplanar, non-resonant systems of close-in super-Earths |
spellingShingle |
The origins of nearly coplanar, non-resonant systems of close-in super-Earths Esteves, Leandro [UNESP] Planets and satellites: formation Protoplanetary discs |
title_short |
The origins of nearly coplanar, non-resonant systems of close-in super-Earths |
title_full |
The origins of nearly coplanar, non-resonant systems of close-in super-Earths |
title_fullStr |
The origins of nearly coplanar, non-resonant systems of close-in super-Earths |
title_full_unstemmed |
The origins of nearly coplanar, non-resonant systems of close-in super-Earths |
title_sort |
The origins of nearly coplanar, non-resonant systems of close-in super-Earths |
author |
Esteves, Leandro [UNESP] |
author_facet |
Esteves, Leandro [UNESP] Izidoro, André [UNESP] Raymond, Sean N. Bitsch, Bertram |
author_role |
author |
author2 |
Izidoro, André [UNESP] Raymond, Sean N. Bitsch, Bertram |
author2_role |
author author author |
dc.contributor.none.fl_str_mv |
Universidade Estadual Paulista (Unesp) Rice University Cnrs Max-Planck-Institut für Astronomie |
dc.contributor.author.fl_str_mv |
Esteves, Leandro [UNESP] Izidoro, André [UNESP] Raymond, Sean N. Bitsch, Bertram |
dc.subject.por.fl_str_mv |
Planets and satellites: formation Protoplanetary discs |
topic |
Planets and satellites: formation Protoplanetary discs |
description |
Some systems of close-in 'super-Earths' contain five or more planets on non-resonant but compact and nearly coplanar orbits. The Kepler-11 system is an iconic representative of this class of system. It is challenging to explain their origins given that planet-disc interactions are thought to be essential to maintain such a high degree of coplanarity, yet these same interactions invariably cause planets to migrate into chains of mean motion resonances. Here, we mine a large data set of dynamical simulations of super-Earth formation by migration. These simulations match the observed period ratio distribution as long as the vast majority of planet pairs in resonance become dynamically unstable. When instabilities take place resonances are broken during a late phase of giant impacts, and typical surviving systems have planet pairs with significant mutual orbital inclinations. However, a subset of our unstable simulations matches the Kepler-11 system in terms of coplanarity, compactness, planet-multiplicity, and non-resonant state. This subset has dynamical instability phases typically much shorter than ordinary systems. Unstable systems may keep a high degree of coplanarity post-instability if planets collide at very low orbital inclinations (<1°) or if collisions promote efficient damping of orbital inclinations. If planetary scattering during the instability takes place at low orbital inclinations (i < 1°), orbital inclinations are barely increased by encounters before planets collide. When planetary scattering pumps orbital inclinations to higher values (>1°) planets tend to collide at higher mutual orbital inclinations, but depending on the geometry of collisions mergers' orbital inclinations may be efficiently damped. Each of these formation pathways can produce analogues to the Kepler-11 system. |
publishDate |
2020 |
dc.date.none.fl_str_mv |
2020-09-01 2021-06-25T10:15:12Z 2021-06-25T10:15:12Z |
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/staa2112 Monthly Notices of the Royal Astronomical Society, v. 497, n. 2, p. 2493-2500, 2020. 1365-2966 0035-8711 http://hdl.handle.net/11449/205432 10.1093/mnras/staa2112 2-s2.0-85095444023 |
url |
http://dx.doi.org/10.1093/mnras/staa2112 http://hdl.handle.net/11449/205432 |
identifier_str_mv |
Monthly Notices of the Royal Astronomical Society, v. 497, n. 2, p. 2493-2500, 2020. 1365-2966 0035-8711 10.1093/mnras/staa2112 2-s2.0-85095444023 |
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 |
2493-2500 |
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_ |
1808129430192652288 |