Dynamical formation of Gaia BH1 in a young star cluster

Gaia BH1, the first quiescent black hole (BH) detected from Gaia data, poses a challenge to most binary evolution models: its current mass ratio is ≈0.1, and its orbital period seems to be too long for a post-common envelope system and too short for a non-interacting binary system. Here, we explore...

Descripción completa

Detalles Bibliográficos
Autores: Rastello, Sara, Iorio, Giuliano, Mapelli, Michela, Arca-Sedda, Manuel, Di Carlo, Ugo N., Escobar, Gastón J., Shenar, Tomer, Torniamenti, Stefano
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2023
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/347902
Acceso en línea:http://hdl.handle.net/10261/347902
Access Level:acceso abierto
Palabra clave:Black hole physics
Methods: numerical
Binaries: general
Open clusters and associations: general
Stars: kinematics and dynamics
Galaxies: star clusters: general
id ES_acfe4d21fab942aa99562bf092a2ef4d
oai_identifier_str oai:digital.csic.es:10261/347902
network_acronym_str ES
network_name_str España
spelling Dynamical formation of Gaia BH1 in a young star cluster Rastello, Sara Iorio, Giuliano Mapelli, Michela Arca-Sedda, Manuel Di Carlo, Ugo N. Escobar, Gastón J. Shenar, Tomer Torniamenti, Stefano Black hole physics Methods: numerical Binaries: general Open clusters and associations: general Stars: kinematics and dynamics Galaxies: star clusters: general Gaia BH1, the first quiescent black hole (BH) detected from Gaia data, poses a challenge to most binary evolution models: its current mass ratio is ≈0.1, and its orbital period seems to be too long for a post-common envelope system and too short for a non-interacting binary system. Here, we explore the hypothesis that Gaia BH1 formed through dynamical interactions in a young star cluster (YSC). We study the properties of BH-main sequence (MS) binaries formed in YSCs with initial mass 3 × 102–3 × 104 M⊙ at solar metallicity, by means of 3.5 × 104 direct N-body simulations coupled with binary population synthesis. For comparison, we also run a sample of isolated binary stars with the same binary population synthesis code and initial conditions used in the dynamical models. We find that BH-MS systems that form via dynamical exchanges populate the region corresponding to the main orbital properties of Gaia BH1 (period, eccentricity, and masses). In contrast, none of our isolated binary systems match the orbital period and MS mass of Gaia BH1. Our best-matching Gaia BH1-like system forms via repeated dynamical exchanges and collisions involving the BH progenitor star, before it undergoes core collapse. YSCs are at least two orders of magnitude more efficient in forming Gaia BH1-like systems than isolated binary evolution. MM, GE, GI, SR, ST, and UNDC acknowledge financial support from the European Research Council for the ERC Consolidator grant DEMOBLACK, under contract no. 770017. MM also acknowledges financial support from the German Excellence Strategy via the Heidelberg Cluster of Excellence (EXC 2181–390900948) STRUCTURES. MAS acknowledges funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 101025436 (project GRACE-BH). TS was supported by the European Union’s Horizon 2020 Marie Skłodowska-Curie grant No. 101024605. SR acknowledges support from the Beatriu de Pinós postdoctoral program under the Ministry of Reseach and Universities of the Government of Catalonia (Grant Reference No. 2021 BP 00213). This work benefited from support of the Munich Institute for Astro-, Particle, and BioPhysics (MIAPbP), funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy – EXC-2094–390783311. We acknowledge the CINECA-INFN agreement, for the availability of high-performance computing resources and support. Peer reviewed Oxford University Press http://hdl.handle.net/10261/347902
title Dynamical formation of Gaia BH1 in a young star cluster
spellingShingle Dynamical formation of Gaia BH1 in a young star cluster
Rastello, Sara
Black hole physics
Methods: numerical
Binaries: general
Open clusters and associations: general
Stars: kinematics and dynamics
Galaxies: star clusters: general
title_short Dynamical formation of Gaia BH1 in a young star cluster
title_full Dynamical formation of Gaia BH1 in a young star cluster
title_fullStr Dynamical formation of Gaia BH1 in a young star cluster
title_full_unstemmed Dynamical formation of Gaia BH1 in a young star cluster
title_sort Dynamical formation of Gaia BH1 in a young star cluster
author Rastello, Sara
author_facet Rastello, Sara
Iorio, Giuliano
Mapelli, Michela
Arca-Sedda, Manuel
Di Carlo, Ugo N.
Escobar, Gastón J.
Shenar, Tomer
Torniamenti, Stefano
author_role author
author2 Iorio, Giuliano
Mapelli, Michela
Arca-Sedda, Manuel
Di Carlo, Ugo N.
Escobar, Gastón J.
Shenar, Tomer
Torniamenti, Stefano
author2_role author
author
author
author
author
author
author
topic Black hole physics
Methods: numerical
Binaries: general
Open clusters and associations: general
Stars: kinematics and dynamics
Galaxies: star clusters: general
topic_facet Black hole physics
Methods: numerical
Binaries: general
Open clusters and associations: general
Stars: kinematics and dynamics
Galaxies: star clusters: general
description Gaia BH1, the first quiescent black hole (BH) detected from Gaia data, poses a challenge to most binary evolution models: its current mass ratio is ≈0.1, and its orbital period seems to be too long for a post-common envelope system and too short for a non-interacting binary system. Here, we explore the hypothesis that Gaia BH1 formed through dynamical interactions in a young star cluster (YSC). We study the properties of BH-main sequence (MS) binaries formed in YSCs with initial mass 3 × 102–3 × 104 M⊙ at solar metallicity, by means of 3.5 × 104 direct N-body simulations coupled with binary population synthesis. For comparison, we also run a sample of isolated binary stars with the same binary population synthesis code and initial conditions used in the dynamical models. We find that BH-MS systems that form via dynamical exchanges populate the region corresponding to the main orbital properties of Gaia BH1 (period, eccentricity, and masses). In contrast, none of our isolated binary systems match the orbital period and MS mass of Gaia BH1. Our best-matching Gaia BH1-like system forms via repeated dynamical exchanges and collisions involving the BH progenitor star, before it undergoes core collapse. YSCs are at least two orders of magnitude more efficient in forming Gaia BH1-like systems than isolated binary evolution.
publishDate 2023
format article
status_str publishedVersion
url http://hdl.handle.net/10261/347902
eu_rights_str_mv openAccess
publisher Oxford University Press
institution Consejo Superior de Investigaciones Científicas (CSIC)
collection DIGITAL.CSIC. Repositorio Institucional del CSIC
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
_version_ 1878439263633145856
publishDateSort 2023
author_browse Arca-Sedda, Manuel
Di Carlo, Ugo N.
Escobar, Gastón J.
Iorio, Giuliano
Mapelli, Michela
Rastello, Sara
Shenar, Tomer
Torniamenti, Stefano
publisherStr Oxford University Press
score 6,9303427

Similares en LA Referencia