Dependence of Planet Populations on Stellar Mass and Metallicity: A Pebble-accretion-based Planet Population Synthesis Model

The formation and evolution of planetary systems are linked to their host stellar environment. In this study, we employ a pebble-accretion-based planet population synthesis model to explore the correlation between planetary properties and stellar mass/metallicity. Our numerical results reproduce sev...

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Detalles Bibliográficos
Autores: Pan, Mengrui, Liu, Beibei, Jiang, Linjie, Xie, Jiwei, Zhu, Wei, Ribas, Ignasi
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2025
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/391177
Acceso en línea:http://hdl.handle.net/10261/391177
https://api.elsevier.com/content/abstract/scopus_id/105004885777
Access Level:acceso abierto
Palabra clave:Exoplanet dynamics
Exoplanets
Exoplanet systems
Exoplanet migration
Exoplanet formation
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spelling Dependence of Planet Populations on Stellar Mass and Metallicity: A Pebble-accretion-based Planet Population Synthesis ModelPan, MengruiLiu, BeibeiJiang, LinjieXie, JiweiZhu, WeiRibas, IgnasiExoplanet dynamicsExoplanetsExoplanet systemsExoplanet migrationExoplanet formationThe formation and evolution of planetary systems are linked to their host stellar environment. In this study, we employ a pebble-accretion-based planet population synthesis model to explore the correlation between planetary properties and stellar mass/metallicity. Our numerical results reproduce several main aspects of exoplanetary observations. First, we find that the occurrence rate of super-Earths, ηSE, follows an inverted V-shape in relation to stellar mass: it increases with stellar mass among lower-mass dwarfs, peaks at early M dwarfs, and declines toward higher-mass GK stars. Second, super-Earths grow ubiquitously around stars with various metallicities, exhibiting a flat or weak ηSE dependence on Z⋆. Third, giant planets in contrast form more frequently around stars with higher mass/metallicity. Lastly, we extend a subset of simulations to 1 Gyr to investigate the long-term evolution of the systems’ architecture. By converting our simulated systems into synthetic observations, we find that the eccentricities and inclinations of single-transit systems increase with stellar metallicity, while these dependencies in multiplanet systems remains relatively weak. The alignment between our results and observations provides key insights into the connection between planet populations and stellar properties.This work is supported by the National Key R&D Program of China (grant No. 2024YFA1611803). B.L. and M.P. are supported by National Natural Science Foundation of China (grant Nos. 12222303, 12173035, and 12111530175), a start-up grant of the Bairen program from Zhejiang University and the Fundamental Research Funds for the Central Universities (grant No.2022-KYY-506107- 0001,226-2022-00216). J.-W. X. also acknowledges the support from the National Youth Talent Support Program W.Z. acknowledges National Natural Science Foundation of China (grant Nos. 12173021 and 12133005). I.R. acknowledges further financial support from the European Research Council (ERC) under the European Union's Horizon Europe program (ERC Advanced grant SPOTLESS, No. 101140786). The simulations and analysis presented in this article were both carried out on the SilkRiver Supercomputer of Zhejiang University and high-performance computing cluster from the Purple Mountain Observatory of the Chinese Academy of Sciences.Peer reviewedIOP PublishingAmerican Astronomical SocietyNational Key Research and Development Program (China)National Natural Science Foundation of ChinaZhejiang UniversityFundamental Research Funds for the Central Universities (China)European Research CouncilEuropean CommissionPan, Mengrui [0000-0002-0162-163X]Liu, Beibei [0000-0001-5830-3619]Xie, Jiwei [0000-0002-6472-5348]Zhu, Wei [0000-0003-4027-4711]Ribas, Ignasi [0000-0002-6689-0312]Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202520252025info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionapplication/pdfhttp://hdl.handle.net/10261/391177https://api.elsevier.com/content/abstract/scopus_id/105004885777reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/EC/H2020/101140786https://doi.org/10.3847/1538-4357/adc7a9Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/3911772026-05-22T06:33:51Z
dc.title.none.fl_str_mv Dependence of Planet Populations on Stellar Mass and Metallicity: A Pebble-accretion-based Planet Population Synthesis Model
title Dependence of Planet Populations on Stellar Mass and Metallicity: A Pebble-accretion-based Planet Population Synthesis Model
spellingShingle Dependence of Planet Populations on Stellar Mass and Metallicity: A Pebble-accretion-based Planet Population Synthesis Model
Pan, Mengrui
Exoplanet dynamics
Exoplanets
Exoplanet systems
Exoplanet migration
Exoplanet formation
title_short Dependence of Planet Populations on Stellar Mass and Metallicity: A Pebble-accretion-based Planet Population Synthesis Model
title_full Dependence of Planet Populations on Stellar Mass and Metallicity: A Pebble-accretion-based Planet Population Synthesis Model
title_fullStr Dependence of Planet Populations on Stellar Mass and Metallicity: A Pebble-accretion-based Planet Population Synthesis Model
title_full_unstemmed Dependence of Planet Populations on Stellar Mass and Metallicity: A Pebble-accretion-based Planet Population Synthesis Model
title_sort Dependence of Planet Populations on Stellar Mass and Metallicity: A Pebble-accretion-based Planet Population Synthesis Model
dc.creator.none.fl_str_mv Pan, Mengrui
Liu, Beibei
Jiang, Linjie
Xie, Jiwei
Zhu, Wei
Ribas, Ignasi
author Pan, Mengrui
author_facet Pan, Mengrui
Liu, Beibei
Jiang, Linjie
Xie, Jiwei
Zhu, Wei
Ribas, Ignasi
author_role author
author2 Liu, Beibei
Jiang, Linjie
Xie, Jiwei
Zhu, Wei
Ribas, Ignasi
author2_role author
author
author
author
author
dc.contributor.none.fl_str_mv National Key Research and Development Program (China)
National Natural Science Foundation of China
Zhejiang University
Fundamental Research Funds for the Central Universities (China)
European Research Council
European Commission
Pan, Mengrui [0000-0002-0162-163X]
Liu, Beibei [0000-0001-5830-3619]
Xie, Jiwei [0000-0002-6472-5348]
Zhu, Wei [0000-0003-4027-4711]
Ribas, Ignasi [0000-0002-6689-0312]
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Exoplanet dynamics
Exoplanets
Exoplanet systems
Exoplanet migration
Exoplanet formation
topic Exoplanet dynamics
Exoplanets
Exoplanet systems
Exoplanet migration
Exoplanet formation
description The formation and evolution of planetary systems are linked to their host stellar environment. In this study, we employ a pebble-accretion-based planet population synthesis model to explore the correlation between planetary properties and stellar mass/metallicity. Our numerical results reproduce several main aspects of exoplanetary observations. First, we find that the occurrence rate of super-Earths, ηSE, follows an inverted V-shape in relation to stellar mass: it increases with stellar mass among lower-mass dwarfs, peaks at early M dwarfs, and declines toward higher-mass GK stars. Second, super-Earths grow ubiquitously around stars with various metallicities, exhibiting a flat or weak ηSE dependence on Z⋆. Third, giant planets in contrast form more frequently around stars with higher mass/metallicity. Lastly, we extend a subset of simulations to 1 Gyr to investigate the long-term evolution of the systems’ architecture. By converting our simulated systems into synthetic observations, we find that the eccentricities and inclinations of single-transit systems increase with stellar metallicity, while these dependencies in multiplanet systems remains relatively weak. The alignment between our results and observations provides key insights into the connection between planet populations and stellar properties.
publishDate 2025
dc.date.none.fl_str_mv 2025
2025
2025
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Publisher's version
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/391177
https://api.elsevier.com/content/abstract/scopus_id/105004885777
url http://hdl.handle.net/10261/391177
https://api.elsevier.com/content/abstract/scopus_id/105004885777
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
info:eu-repo/grantAgreement/EC/H2020/101140786
https://doi.org/10.3847/1538-4357/adc7a9
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv IOP Publishing
American Astronomical Society
publisher.none.fl_str_mv IOP Publishing
American Astronomical Society
dc.source.none.fl_str_mv reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC
instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
collection DIGITAL.CSIC. Repositorio Institucional del CSIC
repository.name.fl_str_mv
repository.mail.fl_str_mv
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