Infalling clouds on to supermassive black hole binaries - I. Formation of discs, accretion and gas dynamics

Autores
Goicovic, Felipe; Cuadra, Jorge; Sesana, A.; Stasyszyn, Federico Andres; Amaro-Seoane, P.; Tanaka, T. L.
Año de publicación
2016
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
There is compelling evidence that most - if not all - galaxies harbour a supermassive black hole (SMBH) at their nucleus; hence binaries of these massive objects are an inevitable product of the hierarchical evolution of structures in the Universe, and represent an important but thus-far elusive phase of galaxy evolution. Gas accretion via a circumbinary disc is thought to be important for the dynamical evolution of SMBH binaries, as well as in producing luminous emission that can be used to infer their properties. One plausible source of the gaseous fuel is clumps of gas formed due to turbulence and gravitational instabilities in the interstellar medium, that later fall towards and interact with the binary. In this context, we model numerically the evolution of turbulent clouds in near-radial infall on to equal-mass SMBH binaries, using a modified version of the SPH (smoothed particle hydrodynamics) code GADGET-3. We present a total of 12 simulations that explore different possible pericentre distances and relative inclinations, and show that the formation of circumbinary discs and discs around each SMBH ('mini-discs') depend on those parameters. We also study the dynamics of the formed discs, and the variability of the feeding rate on to the SMBHs in the different configurations.
Fil: Goicovic, Felipe. Pontificia Universidad Catolica de Chile. Facultad de Física. Departamento de Física; Chile. Max-planck-institut Für Gravitationsphysik; Alemania
Fil: Cuadra, Jorge. Pontificia Universidad Catolica de Chile. Facultad de Física. Departamento de Física; Chile
Fil: Sesana, A.. University of Birmingham. School of Physics and Astronomy; Reino Unido. Max-planck-institut Für Gravitationsphysik; Alemania
Fil: Stasyszyn, Federico Andres. Max-planck Institut Für Gravitationphysick; Alemania. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina
Fil: Amaro-Seoane, P.. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; Alemania
Fil: Tanaka, T. L.. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; Alemania. Washington State University; Estados Unidos. State University of New York. Stony Brook University; Estados Unidos
Materia
ACCRETION
ACCRETION DISCS
BLACK HOLE PHYSICS
GALAXIES: EVOLUTION
GALAXIES: NUCLEI
HYDRODYNAMICS
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/183604
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/183604
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Infalling clouds on to supermassive black hole binaries - I. Formation of discs, accretion and gas dynamicsGoicovic, FelipeCuadra, JorgeSesana, A.Stasyszyn, Federico AndresAmaro-Seoane, P.Tanaka, T. L.ACCRETIONACCRETION DISCSBLACK HOLE PHYSICSGALAXIES: EVOLUTIONGALAXIES: NUCLEIHYDRODYNAMICShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1There is compelling evidence that most - if not all - galaxies harbour a supermassive black hole (SMBH) at their nucleus; hence binaries of these massive objects are an inevitable product of the hierarchical evolution of structures in the Universe, and represent an important but thus-far elusive phase of galaxy evolution. Gas accretion via a circumbinary disc is thought to be important for the dynamical evolution of SMBH binaries, as well as in producing luminous emission that can be used to infer their properties. One plausible source of the gaseous fuel is clumps of gas formed due to turbulence and gravitational instabilities in the interstellar medium, that later fall towards and interact with the binary. In this context, we model numerically the evolution of turbulent clouds in near-radial infall on to equal-mass SMBH binaries, using a modified version of the SPH (smoothed particle hydrodynamics) code GADGET-3. We present a total of 12 simulations that explore different possible pericentre distances and relative inclinations, and show that the formation of circumbinary discs and discs around each SMBH ('mini-discs') depend on those parameters. We also study the dynamics of the formed discs, and the variability of the feeding rate on to the SMBHs in the different configurations.Fil: Goicovic, Felipe. Pontificia Universidad Catolica de Chile. Facultad de Física. Departamento de Física; Chile. Max-planck-institut Für Gravitationsphysik; AlemaniaFil: Cuadra, Jorge. Pontificia Universidad Catolica de Chile. Facultad de Física. Departamento de Física; ChileFil: Sesana, A.. University of Birmingham. School of Physics and Astronomy; Reino Unido. Max-planck-institut Für Gravitationsphysik; AlemaniaFil: Stasyszyn, Federico Andres. Max-planck Institut Für Gravitationphysick; Alemania. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; ArgentinaFil: Amaro-Seoane, P.. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; AlemaniaFil: Tanaka, T. L.. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; Alemania. Washington State University; Estados Unidos. State University of New York. Stony Brook University; Estados UnidosWiley Blackwell Publishing, Inc2016-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/183604Goicovic, Felipe; Cuadra, Jorge; Sesana, A.; Stasyszyn, Federico Andres; Amaro-Seoane, P.; et al.; Infalling clouds on to supermassive black hole binaries - I. Formation of discs, accretion and gas dynamics; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 455; 2; 1-2016; 1989-20030035-87111365-2966CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stv2470info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/455/2/1989/1122366info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:22:26Zoai:ri.conicet.gov.ar:11336/183604instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-29 10:22:26.951CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Infalling clouds on to supermassive black hole binaries - I. Formation of discs, accretion and gas dynamics
title Infalling clouds on to supermassive black hole binaries - I. Formation of discs, accretion and gas dynamics
spellingShingle Infalling clouds on to supermassive black hole binaries - I. Formation of discs, accretion and gas dynamics
Goicovic, Felipe
ACCRETION
ACCRETION DISCS
BLACK HOLE PHYSICS
GALAXIES: EVOLUTION
GALAXIES: NUCLEI
HYDRODYNAMICS
title_short Infalling clouds on to supermassive black hole binaries - I. Formation of discs, accretion and gas dynamics
title_full Infalling clouds on to supermassive black hole binaries - I. Formation of discs, accretion and gas dynamics
title_fullStr Infalling clouds on to supermassive black hole binaries - I. Formation of discs, accretion and gas dynamics
title_full_unstemmed Infalling clouds on to supermassive black hole binaries - I. Formation of discs, accretion and gas dynamics
title_sort Infalling clouds on to supermassive black hole binaries - I. Formation of discs, accretion and gas dynamics
dc.creator.none.fl_str_mv Goicovic, Felipe
Cuadra, Jorge
Sesana, A.
Stasyszyn, Federico Andres
Amaro-Seoane, P.
Tanaka, T. L.
author Goicovic, Felipe
author_facet Goicovic, Felipe
Cuadra, Jorge
Sesana, A.
Stasyszyn, Federico Andres
Amaro-Seoane, P.
Tanaka, T. L.
author_role author
author2 Cuadra, Jorge
Sesana, A.
Stasyszyn, Federico Andres
Amaro-Seoane, P.
Tanaka, T. L.
author2_role author
author
author
author
author
dc.subject.none.fl_str_mv ACCRETION
ACCRETION DISCS
BLACK HOLE PHYSICS
GALAXIES: EVOLUTION
GALAXIES: NUCLEI
HYDRODYNAMICS
topic ACCRETION
ACCRETION DISCS
BLACK HOLE PHYSICS
GALAXIES: EVOLUTION
GALAXIES: NUCLEI
HYDRODYNAMICS
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv There is compelling evidence that most - if not all - galaxies harbour a supermassive black hole (SMBH) at their nucleus; hence binaries of these massive objects are an inevitable product of the hierarchical evolution of structures in the Universe, and represent an important but thus-far elusive phase of galaxy evolution. Gas accretion via a circumbinary disc is thought to be important for the dynamical evolution of SMBH binaries, as well as in producing luminous emission that can be used to infer their properties. One plausible source of the gaseous fuel is clumps of gas formed due to turbulence and gravitational instabilities in the interstellar medium, that later fall towards and interact with the binary. In this context, we model numerically the evolution of turbulent clouds in near-radial infall on to equal-mass SMBH binaries, using a modified version of the SPH (smoothed particle hydrodynamics) code GADGET-3. We present a total of 12 simulations that explore different possible pericentre distances and relative inclinations, and show that the formation of circumbinary discs and discs around each SMBH ('mini-discs') depend on those parameters. We also study the dynamics of the formed discs, and the variability of the feeding rate on to the SMBHs in the different configurations.
Fil: Goicovic, Felipe. Pontificia Universidad Catolica de Chile. Facultad de Física. Departamento de Física; Chile. Max-planck-institut Für Gravitationsphysik; Alemania
Fil: Cuadra, Jorge. Pontificia Universidad Catolica de Chile. Facultad de Física. Departamento de Física; Chile
Fil: Sesana, A.. University of Birmingham. School of Physics and Astronomy; Reino Unido. Max-planck-institut Für Gravitationsphysik; Alemania
Fil: Stasyszyn, Federico Andres. Max-planck Institut Für Gravitationphysick; Alemania. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina
Fil: Amaro-Seoane, P.. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; Alemania
Fil: Tanaka, T. L.. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; Alemania. Washington State University; Estados Unidos. State University of New York. Stony Brook University; Estados Unidos
description There is compelling evidence that most - if not all - galaxies harbour a supermassive black hole (SMBH) at their nucleus; hence binaries of these massive objects are an inevitable product of the hierarchical evolution of structures in the Universe, and represent an important but thus-far elusive phase of galaxy evolution. Gas accretion via a circumbinary disc is thought to be important for the dynamical evolution of SMBH binaries, as well as in producing luminous emission that can be used to infer their properties. One plausible source of the gaseous fuel is clumps of gas formed due to turbulence and gravitational instabilities in the interstellar medium, that later fall towards and interact with the binary. In this context, we model numerically the evolution of turbulent clouds in near-radial infall on to equal-mass SMBH binaries, using a modified version of the SPH (smoothed particle hydrodynamics) code GADGET-3. We present a total of 12 simulations that explore different possible pericentre distances and relative inclinations, and show that the formation of circumbinary discs and discs around each SMBH ('mini-discs') depend on those parameters. We also study the dynamics of the formed discs, and the variability of the feeding rate on to the SMBHs in the different configurations.
publishDate 2016
dc.date.none.fl_str_mv 2016-01
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/183604
Goicovic, Felipe; Cuadra, Jorge; Sesana, A.; Stasyszyn, Federico Andres; Amaro-Seoane, P.; et al.; Infalling clouds on to supermassive black hole binaries - I. Formation of discs, accretion and gas dynamics; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 455; 2; 1-2016; 1989-2003
0035-8711
1365-2966
CONICET Digital
CONICET
url http://hdl.handle.net/11336/183604
identifier_str_mv Goicovic, Felipe; Cuadra, Jorge; Sesana, A.; Stasyszyn, Federico Andres; Amaro-Seoane, P.; et al.; Infalling clouds on to supermassive black hole binaries - I. Formation of discs, accretion and gas dynamics; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 455; 2; 1-2016; 1989-2003
0035-8711
1365-2966
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stv2470
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/455/2/1989/1122366
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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score 13.070432

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