The X-ray corona in the black hole binary GRO J1655-40 from the properties of non-harmonically related quasi-periodic oscillations

Autores
Rout, Sandeep K.; Méndez, Mariano; García, Federico
Año de publicación
2023
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The study of quasi-periodic oscillations (QPOs) plays a vital role in understanding the nature and geometry of the Comptonizing medium around black hole X-ray binaries. The spectral-state dependence of various types of QPOs (namely A, B, and C) suggests that they could have different origins. The simultaneous presence of different types of QPOs would therefore imply the simultaneous occurrence of different mechanisms. In this work, we study the radiative properties of two non-harmonically related QPOs in the black hole binary GRO J1655-40 detected at the peak of the ultraluminous state during the 2005 outburst of the source. The two QPOs have been previously identified as types B and C, respectively. We jointly fit the phase-lag and rms spectra of the QPOs and the time-averaged spectrum of the source with the time-dependent Comptonization model vkompth to infer the geometry of the media producing the QPOs. The time-averaged spectrum required a hot disc of 2.3 keV and a steep power law with index 2.7, revealing that the source was in an ultraluminous state. The corona that drives the variability of the type-B QPO is smaller in size and has a lower feedback fraction than the one that drives the variability of the type-C QPO. This suggests the simultaneous presence of a horizontally extended corona covering the accretion disc and a vertically elongated jet-like corona that are responsible for the type-C and B QPOs, respectively.
Fil: Rout, Sandeep K.. Physical Research Laboratory India; India
Fil: Méndez, Mariano. University of Groningen; Países Bajos
Fil: García, Federico. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Materia
ACCRETION
ACCRETION DISCS - STARS: BLACK HOLES - STARS: INDIVIDUAL: GRO J1655-40
X-RAYS: BINARIES
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:11336/231315
Acceder
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network_name_str CONICET Digital (CONICET)
spelling The X-ray corona in the black hole binary GRO J1655-40 from the properties of non-harmonically related quasi-periodic oscillationsRout, Sandeep K.Méndez, MarianoGarcía, FedericoACCRETIONACCRETION DISCS - STARS: BLACK HOLES - STARS: INDIVIDUAL: GRO J1655-40X-RAYS: BINARIEShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The study of quasi-periodic oscillations (QPOs) plays a vital role in understanding the nature and geometry of the Comptonizing medium around black hole X-ray binaries. The spectral-state dependence of various types of QPOs (namely A, B, and C) suggests that they could have different origins. The simultaneous presence of different types of QPOs would therefore imply the simultaneous occurrence of different mechanisms. In this work, we study the radiative properties of two non-harmonically related QPOs in the black hole binary GRO J1655-40 detected at the peak of the ultraluminous state during the 2005 outburst of the source. The two QPOs have been previously identified as types B and C, respectively. We jointly fit the phase-lag and rms spectra of the QPOs and the time-averaged spectrum of the source with the time-dependent Comptonization model vkompth to infer the geometry of the media producing the QPOs. The time-averaged spectrum required a hot disc of 2.3 keV and a steep power law with index 2.7, revealing that the source was in an ultraluminous state. The corona that drives the variability of the type-B QPO is smaller in size and has a lower feedback fraction than the one that drives the variability of the type-C QPO. This suggests the simultaneous presence of a horizontally extended corona covering the accretion disc and a vertically elongated jet-like corona that are responsible for the type-C and B QPOs, respectively.Fil: Rout, Sandeep K.. Physical Research Laboratory India; IndiaFil: Méndez, Mariano. University of Groningen; Países BajosFil: García, Federico. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; ArgentinaWiley Blackwell Publishing, Inc2023-10info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/231315Rout, Sandeep K.; Méndez, Mariano; García, Federico; The X-ray corona in the black hole binary GRO J1655-40 from the properties of non-harmonically related quasi-periodic oscillations; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 525; 1; 10-2023; 221-2300035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stad2321info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/525/1/221/7236050info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:28:50Zoai:ri.conicet.gov.ar:11336/231315instacron: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:34982025-10-22 11:28:50.589CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The X-ray corona in the black hole binary GRO J1655-40 from the properties of non-harmonically related quasi-periodic oscillations
title The X-ray corona in the black hole binary GRO J1655-40 from the properties of non-harmonically related quasi-periodic oscillations
spellingShingle The X-ray corona in the black hole binary GRO J1655-40 from the properties of non-harmonically related quasi-periodic oscillations
Rout, Sandeep K.
ACCRETION
ACCRETION DISCS - STARS: BLACK HOLES - STARS: INDIVIDUAL: GRO J1655-40
X-RAYS: BINARIES
title_short The X-ray corona in the black hole binary GRO J1655-40 from the properties of non-harmonically related quasi-periodic oscillations
title_full The X-ray corona in the black hole binary GRO J1655-40 from the properties of non-harmonically related quasi-periodic oscillations
title_fullStr The X-ray corona in the black hole binary GRO J1655-40 from the properties of non-harmonically related quasi-periodic oscillations
title_full_unstemmed The X-ray corona in the black hole binary GRO J1655-40 from the properties of non-harmonically related quasi-periodic oscillations
title_sort The X-ray corona in the black hole binary GRO J1655-40 from the properties of non-harmonically related quasi-periodic oscillations
dc.creator.none.fl_str_mv Rout, Sandeep K.
Méndez, Mariano
García, Federico
author Rout, Sandeep K.
author_facet Rout, Sandeep K.
Méndez, Mariano
García, Federico
author_role author
author2 Méndez, Mariano
García, Federico
author2_role author
author
dc.subject.none.fl_str_mv ACCRETION
ACCRETION DISCS - STARS: BLACK HOLES - STARS: INDIVIDUAL: GRO J1655-40
X-RAYS: BINARIES
topic ACCRETION
ACCRETION DISCS - STARS: BLACK HOLES - STARS: INDIVIDUAL: GRO J1655-40
X-RAYS: BINARIES
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv The study of quasi-periodic oscillations (QPOs) plays a vital role in understanding the nature and geometry of the Comptonizing medium around black hole X-ray binaries. The spectral-state dependence of various types of QPOs (namely A, B, and C) suggests that they could have different origins. The simultaneous presence of different types of QPOs would therefore imply the simultaneous occurrence of different mechanisms. In this work, we study the radiative properties of two non-harmonically related QPOs in the black hole binary GRO J1655-40 detected at the peak of the ultraluminous state during the 2005 outburst of the source. The two QPOs have been previously identified as types B and C, respectively. We jointly fit the phase-lag and rms spectra of the QPOs and the time-averaged spectrum of the source with the time-dependent Comptonization model vkompth to infer the geometry of the media producing the QPOs. The time-averaged spectrum required a hot disc of 2.3 keV and a steep power law with index 2.7, revealing that the source was in an ultraluminous state. The corona that drives the variability of the type-B QPO is smaller in size and has a lower feedback fraction than the one that drives the variability of the type-C QPO. This suggests the simultaneous presence of a horizontally extended corona covering the accretion disc and a vertically elongated jet-like corona that are responsible for the type-C and B QPOs, respectively.
Fil: Rout, Sandeep K.. Physical Research Laboratory India; India
Fil: Méndez, Mariano. University of Groningen; Países Bajos
Fil: García, Federico. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
description The study of quasi-periodic oscillations (QPOs) plays a vital role in understanding the nature and geometry of the Comptonizing medium around black hole X-ray binaries. The spectral-state dependence of various types of QPOs (namely A, B, and C) suggests that they could have different origins. The simultaneous presence of different types of QPOs would therefore imply the simultaneous occurrence of different mechanisms. In this work, we study the radiative properties of two non-harmonically related QPOs in the black hole binary GRO J1655-40 detected at the peak of the ultraluminous state during the 2005 outburst of the source. The two QPOs have been previously identified as types B and C, respectively. We jointly fit the phase-lag and rms spectra of the QPOs and the time-averaged spectrum of the source with the time-dependent Comptonization model vkompth to infer the geometry of the media producing the QPOs. The time-averaged spectrum required a hot disc of 2.3 keV and a steep power law with index 2.7, revealing that the source was in an ultraluminous state. The corona that drives the variability of the type-B QPO is smaller in size and has a lower feedback fraction than the one that drives the variability of the type-C QPO. This suggests the simultaneous presence of a horizontally extended corona covering the accretion disc and a vertically elongated jet-like corona that are responsible for the type-C and B QPOs, respectively.
publishDate 2023
dc.date.none.fl_str_mv 2023-10
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/11336/231315
Rout, Sandeep K.; Méndez, Mariano; García, Federico; The X-ray corona in the black hole binary GRO J1655-40 from the properties of non-harmonically related quasi-periodic oscillations; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 525; 1; 10-2023; 221-230
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/231315
identifier_str_mv Rout, Sandeep K.; Méndez, Mariano; García, Federico; The X-ray corona in the black hole binary GRO J1655-40 from the properties of non-harmonically related quasi-periodic oscillations; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 525; 1; 10-2023; 221-230
0035-8711
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/stad2321
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/525/1/221/7236050
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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