Assessing the spin-orbit obliquity of low-mass planets in the breaking the chain formation model: a story of misalignment
Autor(a) principal: | |
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Data de Publicação: | 2023 |
Outros Autores: | , , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UNESP |
Texto Completo: | http://dx.doi.org/10.1093/mnras/stad756 http://hdl.handle.net/11449/249964 |
Resumo: | The spin-orbit obliquity of a planetary system constraints its formation history. A large obliquity may either indicate a primordial misalignment between the star and its gaseous disc or reflect the effect of different mechanisms tilting planetary systems after formation. Observations and statistical analysis suggest that system of planets with sizes between 1 and 4 R has a wide range of obliquities (∼0-30°), and that single- and multiplanet transiting have statistically indistinguishable obliquity distributions. Here, we revisit the 'breaking the chains' formation model with focus in understanding the origin of spin-orbit obliquities. This model suggests that super-Earths and mini-Neptunes migrate close to their host stars via planet-disc gravitational interactions, forming chain of planets locked in mean-motion resonances. After gas-disc dispersal, about 90-99 per cent of these planetary systems experience dynamical instabilities, which spread the systems out. Using synthetic transit observations, we show that if planets are born in discs where the disc angular momentum is virtually aligned with the star's rotation spin, their final obliquity distributions peak at ∼5° or less, and the obliquity distributions of single- and multiplanet transiting systems are statistically distinct. By treating the star-disc alignment as a free-parameter, we show that the obliquity distributions of single- and multiplanet transiting systems only become statistically indistinguishable if planets are assumed to form in primordially misaligned natal discs with a tilt' distribution peaking at ≥10-20°. We discuss the origin of these misalignments in the context of star formation and potential implications of this scenario for formation models. |
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Assessing the spin-orbit obliquity of low-mass planets in the breaking the chain formation model: a story of misalignmentplanet-disc interactionsplanets and satellites: dynamical evolution and stabilityplanets and satellites: formations and satellitesprotoplanetary discsstars: statisticsThe spin-orbit obliquity of a planetary system constraints its formation history. A large obliquity may either indicate a primordial misalignment between the star and its gaseous disc or reflect the effect of different mechanisms tilting planetary systems after formation. Observations and statistical analysis suggest that system of planets with sizes between 1 and 4 R has a wide range of obliquities (∼0-30°), and that single- and multiplanet transiting have statistically indistinguishable obliquity distributions. Here, we revisit the 'breaking the chains' formation model with focus in understanding the origin of spin-orbit obliquities. This model suggests that super-Earths and mini-Neptunes migrate close to their host stars via planet-disc gravitational interactions, forming chain of planets locked in mean-motion resonances. After gas-disc dispersal, about 90-99 per cent of these planetary systems experience dynamical instabilities, which spread the systems out. Using synthetic transit observations, we show that if planets are born in discs where the disc angular momentum is virtually aligned with the star's rotation spin, their final obliquity distributions peak at ∼5° or less, and the obliquity distributions of single- and multiplanet transiting systems are statistically distinct. By treating the star-disc alignment as a free-parameter, we show that the obliquity distributions of single- and multiplanet transiting systems only become statistically indistinguishable if planets are assumed to form in primordially misaligned natal discs with a tilt' distribution peaking at ≥10-20°. We discuss the origin of these misalignments in the context of star formation and potential implications of this scenario for formation models.Unesp São Paulo State University Grupo de Dinâmica Orbital e Planetologia, SPDepartment of Earth Environmental and Planetary Sciences Rice University, 6100 Main MS 126Department of Physics and Astronomy Rice University, 6100 Main MS-550Max-Planck-Institut für Astronomie, Königstuhl 17Unesp São Paulo State University Grupo de Dinâmica Orbital e Planetologia, SPUniversidade Estadual Paulista (UNESP)Rice UniversityMax-Planck-Institut für AstronomieEsteves, Leandro [UNESP]Izidoro, AndréWinter, Othon C [UNESP]Bitsch, BertramIsella, Andrea2023-07-29T16:14:05Z2023-07-29T16:14:05Z2023-06-01info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/article5776-5785http://dx.doi.org/10.1093/mnras/stad756Monthly Notices of the Royal Astronomical Society, v. 521, n. 4, p. 5776-5785, 2023.1365-29660035-8711http://hdl.handle.net/11449/24996410.1093/mnras/stad7562-s2.0-85159656474Scopusreponame:Repositório Institucional da UNESPinstname:Universidade Estadual Paulista (UNESP)instacron:UNESPengMonthly Notices of the Royal Astronomical Societyinfo:eu-repo/semantics/openAccess2024-07-02T14:29:31Zoai:repositorio.unesp.br:11449/249964Repositório InstitucionalPUBhttp://repositorio.unesp.br/oai/requestopendoar:29462024-08-05T22:22:55.500558Repositório Institucional da UNESP - Universidade Estadual Paulista (UNESP)false |
dc.title.none.fl_str_mv |
Assessing the spin-orbit obliquity of low-mass planets in the breaking the chain formation model: a story of misalignment |
title |
Assessing the spin-orbit obliquity of low-mass planets in the breaking the chain formation model: a story of misalignment |
spellingShingle |
Assessing the spin-orbit obliquity of low-mass planets in the breaking the chain formation model: a story of misalignment Esteves, Leandro [UNESP] planet-disc interactions planets and satellites: dynamical evolution and stability planets and satellites: formations and satellites protoplanetary discs stars: statistics |
title_short |
Assessing the spin-orbit obliquity of low-mass planets in the breaking the chain formation model: a story of misalignment |
title_full |
Assessing the spin-orbit obliquity of low-mass planets in the breaking the chain formation model: a story of misalignment |
title_fullStr |
Assessing the spin-orbit obliquity of low-mass planets in the breaking the chain formation model: a story of misalignment |
title_full_unstemmed |
Assessing the spin-orbit obliquity of low-mass planets in the breaking the chain formation model: a story of misalignment |
title_sort |
Assessing the spin-orbit obliquity of low-mass planets in the breaking the chain formation model: a story of misalignment |
author |
Esteves, Leandro [UNESP] |
author_facet |
Esteves, Leandro [UNESP] Izidoro, André Winter, Othon C [UNESP] Bitsch, Bertram Isella, Andrea |
author_role |
author |
author2 |
Izidoro, André Winter, Othon C [UNESP] Bitsch, Bertram Isella, Andrea |
author2_role |
author author author author |
dc.contributor.none.fl_str_mv |
Universidade Estadual Paulista (UNESP) Rice University Max-Planck-Institut für Astronomie |
dc.contributor.author.fl_str_mv |
Esteves, Leandro [UNESP] Izidoro, André Winter, Othon C [UNESP] Bitsch, Bertram Isella, Andrea |
dc.subject.por.fl_str_mv |
planet-disc interactions planets and satellites: dynamical evolution and stability planets and satellites: formations and satellites protoplanetary discs stars: statistics |
topic |
planet-disc interactions planets and satellites: dynamical evolution and stability planets and satellites: formations and satellites protoplanetary discs stars: statistics |
description |
The spin-orbit obliquity of a planetary system constraints its formation history. A large obliquity may either indicate a primordial misalignment between the star and its gaseous disc or reflect the effect of different mechanisms tilting planetary systems after formation. Observations and statistical analysis suggest that system of planets with sizes between 1 and 4 R has a wide range of obliquities (∼0-30°), and that single- and multiplanet transiting have statistically indistinguishable obliquity distributions. Here, we revisit the 'breaking the chains' formation model with focus in understanding the origin of spin-orbit obliquities. This model suggests that super-Earths and mini-Neptunes migrate close to their host stars via planet-disc gravitational interactions, forming chain of planets locked in mean-motion resonances. After gas-disc dispersal, about 90-99 per cent of these planetary systems experience dynamical instabilities, which spread the systems out. Using synthetic transit observations, we show that if planets are born in discs where the disc angular momentum is virtually aligned with the star's rotation spin, their final obliquity distributions peak at ∼5° or less, and the obliquity distributions of single- and multiplanet transiting systems are statistically distinct. By treating the star-disc alignment as a free-parameter, we show that the obliquity distributions of single- and multiplanet transiting systems only become statistically indistinguishable if planets are assumed to form in primordially misaligned natal discs with a tilt' distribution peaking at ≥10-20°. We discuss the origin of these misalignments in the context of star formation and potential implications of this scenario for formation models. |
publishDate |
2023 |
dc.date.none.fl_str_mv |
2023-07-29T16:14:05Z 2023-07-29T16:14:05Z 2023-06-01 |
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/stad756 Monthly Notices of the Royal Astronomical Society, v. 521, n. 4, p. 5776-5785, 2023. 1365-2966 0035-8711 http://hdl.handle.net/11449/249964 10.1093/mnras/stad756 2-s2.0-85159656474 |
url |
http://dx.doi.org/10.1093/mnras/stad756 http://hdl.handle.net/11449/249964 |
identifier_str_mv |
Monthly Notices of the Royal Astronomical Society, v. 521, n. 4, p. 5776-5785, 2023. 1365-2966 0035-8711 10.1093/mnras/stad756 2-s2.0-85159656474 |
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 |
5776-5785 |
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_ |
1808129421813481472 |