Formation of planetary systems by pebble accretion and migration: Hot super-Earth systems from breaking compact resonant chains
Autor(a) principal: | |
---|---|
Data de Publicação: | 2021 |
Outros Autores: | , , , , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UNESP |
Texto Completo: | http://dx.doi.org/10.1051/0004-6361/201935336 http://hdl.handle.net/11449/221742 |
Resumo: | At least 30% of main sequence stars host planets with sizes of between 1 and 4 Earth radii and orbital periods of less than 100 days.We use N-body simulations including a model for gas-assisted pebble accretion and disk–planet tidal interaction to study the formation of super-Earth systems.We show that the integrated pebble mass reservoir creates a bifurcation between hot super-Earths or hot-Neptunes (.15M) and super-massive planetary cores potentially able to become gas giant planets (&15M). Simulations with moderate pebble fluxes grow multiple super-Earth-mass planets that migrate inwards and pile up at the inner edge of the disk forming long resonant chains. We follow the long-term dynamical evolution of these systems and use the period ratio distribution of observed planet-pairs to constrain our model. Up to 95% of resonant chains become dynamically unstable after the gas disk dispersal, leading to a phase of late collisions that breaks the original resonant configurations. Our simulations naturally match observations when they produce a dominant fraction (&95%) of unstable systems with a sprinkling (.5%) of stable resonant chains (the Trappist-1 system represents one such example). Our results demonstrate that super-Earth systems are inherently multiple (N-2) and that the observed excess of single-planet transits is a consequence of the mutual inclinations excited by the planet–planet instability. In simulations in which planetary seeds are initially distributed in the inner and outer disk, close-in super-Earths are systematically ice rich. This contrasts with the interpretation that most super-Earths are rocky based on bulk-density measurements of super-Earths and photo-evaporation modeling of their bimodal radius distribution.We investigate the conditions needed to form rocky super-Earths. The formation of rocky super-Earths requires special circumstances, such as far more efficient planetesimal formation well inside the snow line, or much faster planetary growth by pebble accretion in the inner disk. Intriguingly, the necessary conditions to match the bulk of hot super-Earths are at odds with the conditions needed to match the Solar System. |
id |
UNSP_d541ee8c13ee68fa269b815be1e4a9be |
---|---|
oai_identifier_str |
oai:repositorio.unesp.br:11449/221742 |
network_acronym_str |
UNSP |
network_name_str |
Repositório Institucional da UNESP |
repository_id_str |
2946 |
spelling |
Formation of planetary systems by pebble accretion and migration: Hot super-Earth systems from breaking compact resonant chainsMethods: numericalPlanet-disk interactionsPlanets and satellites: compositionPlanets and satellites: detectionPlanets and satellites: dynamical evolution and stabilityPlanets and satellites: formationAt least 30% of main sequence stars host planets with sizes of between 1 and 4 Earth radii and orbital periods of less than 100 days.We use N-body simulations including a model for gas-assisted pebble accretion and disk–planet tidal interaction to study the formation of super-Earth systems.We show that the integrated pebble mass reservoir creates a bifurcation between hot super-Earths or hot-Neptunes (.15M) and super-massive planetary cores potentially able to become gas giant planets (&15M). Simulations with moderate pebble fluxes grow multiple super-Earth-mass planets that migrate inwards and pile up at the inner edge of the disk forming long resonant chains. We follow the long-term dynamical evolution of these systems and use the period ratio distribution of observed planet-pairs to constrain our model. Up to 95% of resonant chains become dynamically unstable after the gas disk dispersal, leading to a phase of late collisions that breaks the original resonant configurations. Our simulations naturally match observations when they produce a dominant fraction (&95%) of unstable systems with a sprinkling (.5%) of stable resonant chains (the Trappist-1 system represents one such example). Our results demonstrate that super-Earth systems are inherently multiple (N-2) and that the observed excess of single-planet transits is a consequence of the mutual inclinations excited by the planet–planet instability. In simulations in which planetary seeds are initially distributed in the inner and outer disk, close-in super-Earths are systematically ice rich. This contrasts with the interpretation that most super-Earths are rocky based on bulk-density measurements of super-Earths and photo-evaporation modeling of their bimodal radius distribution.We investigate the conditions needed to form rocky super-Earths. The formation of rocky super-Earths requires special circumstances, such as far more efficient planetesimal formation well inside the snow line, or much faster planetary growth by pebble accretion in the inner disk. Intriguingly, the necessary conditions to match the bulk of hot super-Earths are at odds with the conditions needed to match the Solar System.UNESP Univ. Estadual Paulista - Grupo de Dinâmica Orbital and Planetologia, GuaratinguetáMax-Planck-Institut für Astronomie, Königstuhl 17Laboratoire d'Astrophysique de Bordeaux Univ. Bordeaux CNRS, B18N allée Geoffroy Saint-HilaireLund Observatory Department of Astronomy and Theoretical Physics Lund University, Box 43Laboratoire Lagrange UMR7293 Université Côte d'Azur CNRS Observatoire de la Côte d'Azur, Boulevard de l'ObservatoireDepartment of Earth and Environmental Sciences Michigan State UniversityUNESP Univ. Estadual Paulista - Grupo de Dinâmica Orbital and Planetologia, GuaratinguetáUniversidade Estadual Paulista (UNESP)Max-Planck-Institut für AstronomieCNRSLund UniversityObservatoire de la Côte d'AzurMichigan State UniversityIzidoro, Andre [UNESP]Bitsch, BertramRaymond, Sean N.Johansen, AndersMorbidelli, AlessandroLambrechts, MichielJacobson, Seth A.2022-04-28T19:40:12Z2022-04-28T19:40:12Z2021-06-01info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/articlehttp://dx.doi.org/10.1051/0004-6361/201935336Astronomy and Astrophysics, v. 650.1432-07460004-6361http://hdl.handle.net/11449/22174210.1051/0004-6361/2019353362-s2.0-85105749260Scopusreponame:Repositório Institucional da UNESPinstname:Universidade Estadual Paulista (UNESP)instacron:UNESPengAstronomy and Astrophysicsinfo:eu-repo/semantics/openAccess2022-04-28T19:40:12Zoai:repositorio.unesp.br:11449/221742Repositório InstitucionalPUBhttp://repositorio.unesp.br/oai/requestopendoar:29462024-08-05T17:28:47.448303Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP)false |
dc.title.none.fl_str_mv |
Formation of planetary systems by pebble accretion and migration: Hot super-Earth systems from breaking compact resonant chains |
title |
Formation of planetary systems by pebble accretion and migration: Hot super-Earth systems from breaking compact resonant chains |
spellingShingle |
Formation of planetary systems by pebble accretion and migration: Hot super-Earth systems from breaking compact resonant chains Izidoro, Andre [UNESP] Methods: numerical Planet-disk interactions Planets and satellites: composition Planets and satellites: detection Planets and satellites: dynamical evolution and stability Planets and satellites: formation |
title_short |
Formation of planetary systems by pebble accretion and migration: Hot super-Earth systems from breaking compact resonant chains |
title_full |
Formation of planetary systems by pebble accretion and migration: Hot super-Earth systems from breaking compact resonant chains |
title_fullStr |
Formation of planetary systems by pebble accretion and migration: Hot super-Earth systems from breaking compact resonant chains |
title_full_unstemmed |
Formation of planetary systems by pebble accretion and migration: Hot super-Earth systems from breaking compact resonant chains |
title_sort |
Formation of planetary systems by pebble accretion and migration: Hot super-Earth systems from breaking compact resonant chains |
author |
Izidoro, Andre [UNESP] |
author_facet |
Izidoro, Andre [UNESP] Bitsch, Bertram Raymond, Sean N. Johansen, Anders Morbidelli, Alessandro Lambrechts, Michiel Jacobson, Seth A. |
author_role |
author |
author2 |
Bitsch, Bertram Raymond, Sean N. Johansen, Anders Morbidelli, Alessandro Lambrechts, Michiel Jacobson, Seth A. |
author2_role |
author author author author author author |
dc.contributor.none.fl_str_mv |
Universidade Estadual Paulista (UNESP) Max-Planck-Institut für Astronomie CNRS Lund University Observatoire de la Côte d'Azur Michigan State University |
dc.contributor.author.fl_str_mv |
Izidoro, Andre [UNESP] Bitsch, Bertram Raymond, Sean N. Johansen, Anders Morbidelli, Alessandro Lambrechts, Michiel Jacobson, Seth A. |
dc.subject.por.fl_str_mv |
Methods: numerical Planet-disk interactions Planets and satellites: composition Planets and satellites: detection Planets and satellites: dynamical evolution and stability Planets and satellites: formation |
topic |
Methods: numerical Planet-disk interactions Planets and satellites: composition Planets and satellites: detection Planets and satellites: dynamical evolution and stability Planets and satellites: formation |
description |
At least 30% of main sequence stars host planets with sizes of between 1 and 4 Earth radii and orbital periods of less than 100 days.We use N-body simulations including a model for gas-assisted pebble accretion and disk–planet tidal interaction to study the formation of super-Earth systems.We show that the integrated pebble mass reservoir creates a bifurcation between hot super-Earths or hot-Neptunes (.15M) and super-massive planetary cores potentially able to become gas giant planets (&15M). Simulations with moderate pebble fluxes grow multiple super-Earth-mass planets that migrate inwards and pile up at the inner edge of the disk forming long resonant chains. We follow the long-term dynamical evolution of these systems and use the period ratio distribution of observed planet-pairs to constrain our model. Up to 95% of resonant chains become dynamically unstable after the gas disk dispersal, leading to a phase of late collisions that breaks the original resonant configurations. Our simulations naturally match observations when they produce a dominant fraction (&95%) of unstable systems with a sprinkling (.5%) of stable resonant chains (the Trappist-1 system represents one such example). Our results demonstrate that super-Earth systems are inherently multiple (N-2) and that the observed excess of single-planet transits is a consequence of the mutual inclinations excited by the planet–planet instability. In simulations in which planetary seeds are initially distributed in the inner and outer disk, close-in super-Earths are systematically ice rich. This contrasts with the interpretation that most super-Earths are rocky based on bulk-density measurements of super-Earths and photo-evaporation modeling of their bimodal radius distribution.We investigate the conditions needed to form rocky super-Earths. The formation of rocky super-Earths requires special circumstances, such as far more efficient planetesimal formation well inside the snow line, or much faster planetary growth by pebble accretion in the inner disk. Intriguingly, the necessary conditions to match the bulk of hot super-Earths are at odds with the conditions needed to match the Solar System. |
publishDate |
2021 |
dc.date.none.fl_str_mv |
2021-06-01 2022-04-28T19:40:12Z 2022-04-28T19:40:12Z |
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/10.1051/0004-6361/201935336 Astronomy and Astrophysics, v. 650. 1432-0746 0004-6361 http://hdl.handle.net/11449/221742 10.1051/0004-6361/201935336 2-s2.0-85105749260 |
url |
http://dx.doi.org/10.1051/0004-6361/201935336 http://hdl.handle.net/11449/221742 |
identifier_str_mv |
Astronomy and Astrophysics, v. 650. 1432-0746 0004-6361 10.1051/0004-6361/201935336 2-s2.0-85105749260 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
Astronomy and Astrophysics |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
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_ |
1808128816400302080 |