Bubble-driven gas uplift in galaxy clusters and its velocity features

Buoyant bubbles of relativistic plasma are essential for active galactic nucleus feedback in galaxy clusters, stirring and heating the intracluster medium (ICM). Observations suggest that these rising bubbles maintain their integrity and sharp edges much longer than predicted by hydrodynamic simulat...

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Autores: Zhang, Congyao, Zhuravleva, Irina, Gendron-Marsolais, Marie-Lou, Churazov, Eugene, Schekochihin, Alexander A., Forman, William R.
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2022
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/291094
Acceso en línea:http://hdl.handle.net/10261/291094
Access Level:acceso abierto
Palabra clave:Hydrodynamics
Methods: numerical
Galaxies: clusters: individual: Perseus
Galaxies: clusters: intracluster medium
X-ray galaxy clusters
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spelling Bubble-driven gas uplift in galaxy clusters and its velocity featuresZhang, CongyaoZhuravleva, IrinaGendron-Marsolais, Marie-LouChurazov, EugeneSchekochihin, Alexander A.Forman, William R.HydrodynamicsMethods: numericalGalaxies: clusters: individual: PerseusGalaxies: clusters: intracluster mediumX-ray galaxy clustersBuoyant bubbles of relativistic plasma are essential for active galactic nucleus feedback in galaxy clusters, stirring and heating the intracluster medium (ICM). Observations suggest that these rising bubbles maintain their integrity and sharp edges much longer than predicted by hydrodynamic simulations. In this study, we assume that bubbles can be modelled as rigid bodies and demonstrate that intact bubbles and their long-term interactions with the ambient ICM play an important role in shaping gas kinematics, forming thin gaseous structures (e.g. H α filaments), and generating internal waves in cluster cores. We find that well-developed eddies are formed in the wake of a buoyantly rising bubble, and it is these eddies, rather than the Darwin drift, that are responsible for most of the gas mass uplift. The eddies gradually elongate along the bubble’s direction of motion due to the strong density stratification of the atmosphere and eventually detach from the bubble, quickly evolving into a high-speed jet-like stream propagating towards the cluster center in our model. This picture naturally explains the presence of long straight and horseshoe-shaped H α filaments in the Perseus cluster, inward and outward motions of the gas, and the X-ray-weighted gas velocity distributions near the northwestern bubble observed by Hitomi. Our model reproduces the observed H α velocity structure function of filaments, providing a simple interpretation for its steep scaling and normalization: laminar gas flows and large eddies within filaments driven by the intact bubbles, rather than spatially homogeneous small-scale turbulence, are sufficient to produce a structure function consistent with observations. © 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number TM1-22008X issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. Part of the simulations presented in this paper were carried out using the Midway computing cluster provided by the University of Chicago Research Computing Center. IZ is partially supported by a Clare Boothe Luce Professorship from the Henry Luce Foundation. The work of AAS was supported in part by UK EPSRC grant EP/R034737/1. WF acknowledges support from the Smithsonian Institution, the Chandra High Resolution Camera Project through NASA contract NAS8-03060, and NASA Grants 80NSSC19K0116, GO1-22132X, and GO9-20109X.With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.Peer reviewedOxford University PressMinisterio de Ciencia e Innovación (España)Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202320232022info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/291094reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/MICINN//SEV-2017-0709http://dx.doi.org/10.1093/mnras/stac2282Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/2910942026-05-22T06:33:51Z
dc.title.none.fl_str_mv Bubble-driven gas uplift in galaxy clusters and its velocity features
title Bubble-driven gas uplift in galaxy clusters and its velocity features
spellingShingle Bubble-driven gas uplift in galaxy clusters and its velocity features
Zhang, Congyao
Hydrodynamics
Methods: numerical
Galaxies: clusters: individual: Perseus
Galaxies: clusters: intracluster medium
X-ray galaxy clusters
title_short Bubble-driven gas uplift in galaxy clusters and its velocity features
title_full Bubble-driven gas uplift in galaxy clusters and its velocity features
title_fullStr Bubble-driven gas uplift in galaxy clusters and its velocity features
title_full_unstemmed Bubble-driven gas uplift in galaxy clusters and its velocity features
title_sort Bubble-driven gas uplift in galaxy clusters and its velocity features
dc.creator.none.fl_str_mv Zhang, Congyao
Zhuravleva, Irina
Gendron-Marsolais, Marie-Lou
Churazov, Eugene
Schekochihin, Alexander A.
Forman, William R.
author Zhang, Congyao
author_facet Zhang, Congyao
Zhuravleva, Irina
Gendron-Marsolais, Marie-Lou
Churazov, Eugene
Schekochihin, Alexander A.
Forman, William R.
author_role author
author2 Zhuravleva, Irina
Gendron-Marsolais, Marie-Lou
Churazov, Eugene
Schekochihin, Alexander A.
Forman, William R.
author2_role author
author
author
author
author
dc.contributor.none.fl_str_mv Ministerio de Ciencia e Innovación (España)
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Hydrodynamics
Methods: numerical
Galaxies: clusters: individual: Perseus
Galaxies: clusters: intracluster medium
X-ray galaxy clusters
topic Hydrodynamics
Methods: numerical
Galaxies: clusters: individual: Perseus
Galaxies: clusters: intracluster medium
X-ray galaxy clusters
description Buoyant bubbles of relativistic plasma are essential for active galactic nucleus feedback in galaxy clusters, stirring and heating the intracluster medium (ICM). Observations suggest that these rising bubbles maintain their integrity and sharp edges much longer than predicted by hydrodynamic simulations. In this study, we assume that bubbles can be modelled as rigid bodies and demonstrate that intact bubbles and their long-term interactions with the ambient ICM play an important role in shaping gas kinematics, forming thin gaseous structures (e.g. H α filaments), and generating internal waves in cluster cores. We find that well-developed eddies are formed in the wake of a buoyantly rising bubble, and it is these eddies, rather than the Darwin drift, that are responsible for most of the gas mass uplift. The eddies gradually elongate along the bubble’s direction of motion due to the strong density stratification of the atmosphere and eventually detach from the bubble, quickly evolving into a high-speed jet-like stream propagating towards the cluster center in our model. This picture naturally explains the presence of long straight and horseshoe-shaped H α filaments in the Perseus cluster, inward and outward motions of the gas, and the X-ray-weighted gas velocity distributions near the northwestern bubble observed by Hitomi. Our model reproduces the observed H α velocity structure function of filaments, providing a simple interpretation for its steep scaling and normalization: laminar gas flows and large eddies within filaments driven by the intact bubbles, rather than spatially homogeneous small-scale turbulence, are sufficient to produce a structure function consistent with observations. © 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.
publishDate 2022
dc.date.none.fl_str_mv 2022
2023
2023
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/10261/291094
url http://hdl.handle.net/10261/291094
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/MICINN//SEV-2017-0709
http://dx.doi.org/10.1093/mnras/stac2282
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv Oxford University Press
publisher.none.fl_str_mv Oxford University Press
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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