The evolution of the high-frequency variability in the black hole candidate GRS 1915+105 as seen by RXTE

Autores
Zhang, Yuexin; Mendez, Raul Mariano; García, Federico; Karpouzas, Konstantinos; Zhang, Liang; Liu, Honghui; Belloni, Tomaso M.; Altamirano, Diego
Año de publicación
2022
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
GRS 1915+105 can show type-C quasi-periodic oscillations (QPOs) in the power density spectrum. A high-frequency QPO (HFQPO) at 67 Hz has been observed in this source, albeit less often than the type-C QPOs. Besides these features, GRS 1915+105 sometimes shows a broad bump in the power spectrum at around 30-150 Hz. We study the power spectra of GRS 1915+105 with the Rossi X-ray Timing Explorer when the source was in the χ class. We find that the rms amplitude of the bump depends strongly upon both the frequency of the type-C QPO and the hardness ratio, and is correlated with the corona temperature and anticorrelated with the radio flux at 15 GHz. The characteristic frequency of the bump is better correlated with a combination of the frequency of the type-C QPO and the hardness ratio than with the frequency of the type-C QPO alone. The rms amplitude of the bump generally increases with energy from ∼1-2 per cent at ∼3 keV to ∼10-15 per cent at ∼30 keV. We suggest that the bump and the HFQPO may be the same variability component but the properties of the corona affect the coherence of this variability, leading either to a HFQPO when the spectrum is in the relatively soft γclass, or to a bump when the spectrum is in the hard χ class. Finally, we discuss the anticorrelation between the rms amplitude of the bump and the radio flux in the context of the relation between the corona and the jet.
Fil: Zhang, Yuexin. University of Groningen; Países Bajos
Fil: Mendez, Raul Mariano. University of Groningen; Países Bajos. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
Fil: García, Federico. University of Groningen; Países Bajos. 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
Fil: Karpouzas, Konstantinos. University of Southampton; Reino Unido
Fil: Zhang, Liang. University of Southampton; Reino Unido
Fil: Liu, Honghui. Fudan University; China
Fil: Belloni, Tomaso M.. No especifíca;
Fil: Altamirano, Diego. University of Southampton; Reino Unido
Materia
ACCRETION
ACCRETION DISCS
STARS: BLACK HOLES
STARS: INDIVIDUAL: GRS 1915+105
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:11336/216794
Acceder
id CONICETDig_874154f80e3fe93e29398fc782c63730
oai_identifier_str oai:ri.conicet.gov.ar:11336/216794
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling The evolution of the high-frequency variability in the black hole candidate GRS 1915+105 as seen by RXTEZhang, YuexinMendez, Raul MarianoGarcía, FedericoKarpouzas, KonstantinosZhang, LiangLiu, HonghuiBelloni, Tomaso M.Altamirano, DiegoACCRETIONACCRETION DISCSSTARS: BLACK HOLESSTARS: INDIVIDUAL: GRS 1915+105X-RAYS: BINARIEShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1GRS 1915+105 can show type-C quasi-periodic oscillations (QPOs) in the power density spectrum. A high-frequency QPO (HFQPO) at 67 Hz has been observed in this source, albeit less often than the type-C QPOs. Besides these features, GRS 1915+105 sometimes shows a broad bump in the power spectrum at around 30-150 Hz. We study the power spectra of GRS 1915+105 with the Rossi X-ray Timing Explorer when the source was in the χ class. We find that the rms amplitude of the bump depends strongly upon both the frequency of the type-C QPO and the hardness ratio, and is correlated with the corona temperature and anticorrelated with the radio flux at 15 GHz. The characteristic frequency of the bump is better correlated with a combination of the frequency of the type-C QPO and the hardness ratio than with the frequency of the type-C QPO alone. The rms amplitude of the bump generally increases with energy from ∼1-2 per cent at ∼3 keV to ∼10-15 per cent at ∼30 keV. We suggest that the bump and the HFQPO may be the same variability component but the properties of the corona affect the coherence of this variability, leading either to a HFQPO when the spectrum is in the relatively soft γclass, or to a bump when the spectrum is in the hard χ class. Finally, we discuss the anticorrelation between the rms amplitude of the bump and the radio flux in the context of the relation between the corona and the jet.Fil: Zhang, Yuexin. University of Groningen; Países BajosFil: Mendez, Raul Mariano. University of Groningen; Países Bajos. Consejo Nacional de Investigaciones Científicas y Técnicas; ArgentinaFil: García, Federico. University of Groningen; Países Bajos. 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; ArgentinaFil: Karpouzas, Konstantinos. University of Southampton; Reino UnidoFil: Zhang, Liang. University of Southampton; Reino UnidoFil: Liu, Honghui. Fudan University; ChinaFil: Belloni, Tomaso M.. No especifíca;Fil: Altamirano, Diego. University of Southampton; Reino UnidoWiley Blackwell Publishing, Inc2022-08info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/216794Zhang, Yuexin; Mendez, Raul Mariano; García, Federico; Karpouzas, Konstantinos; Zhang, Liang; et al.; The evolution of the high-frequency variability in the black hole candidate GRS 1915+105 as seen by RXTE; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 514; 2; 8-2022; 2891-29010035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stac1050info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:31:59Zoai:ri.conicet.gov.ar:11336/216794instacron: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 10:31:59.654CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The evolution of the high-frequency variability in the black hole candidate GRS 1915+105 as seen by RXTE
title The evolution of the high-frequency variability in the black hole candidate GRS 1915+105 as seen by RXTE
spellingShingle The evolution of the high-frequency variability in the black hole candidate GRS 1915+105 as seen by RXTE
Zhang, Yuexin
ACCRETION
ACCRETION DISCS
STARS: BLACK HOLES
STARS: INDIVIDUAL: GRS 1915+105
X-RAYS: BINARIES
title_short The evolution of the high-frequency variability in the black hole candidate GRS 1915+105 as seen by RXTE
title_full The evolution of the high-frequency variability in the black hole candidate GRS 1915+105 as seen by RXTE
title_fullStr The evolution of the high-frequency variability in the black hole candidate GRS 1915+105 as seen by RXTE
title_full_unstemmed The evolution of the high-frequency variability in the black hole candidate GRS 1915+105 as seen by RXTE
title_sort The evolution of the high-frequency variability in the black hole candidate GRS 1915+105 as seen by RXTE
dc.creator.none.fl_str_mv Zhang, Yuexin
Mendez, Raul Mariano
García, Federico
Karpouzas, Konstantinos
Zhang, Liang
Liu, Honghui
Belloni, Tomaso M.
Altamirano, Diego
author Zhang, Yuexin
author_facet Zhang, Yuexin
Mendez, Raul Mariano
García, Federico
Karpouzas, Konstantinos
Zhang, Liang
Liu, Honghui
Belloni, Tomaso M.
Altamirano, Diego
author_role author
author2 Mendez, Raul Mariano
García, Federico
Karpouzas, Konstantinos
Zhang, Liang
Liu, Honghui
Belloni, Tomaso M.
Altamirano, Diego
author2_role author
author
author
author
author
author
author
dc.subject.none.fl_str_mv ACCRETION
ACCRETION DISCS
STARS: BLACK HOLES
STARS: INDIVIDUAL: GRS 1915+105
X-RAYS: BINARIES
topic ACCRETION
ACCRETION DISCS
STARS: BLACK HOLES
STARS: INDIVIDUAL: GRS 1915+105
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 GRS 1915+105 can show type-C quasi-periodic oscillations (QPOs) in the power density spectrum. A high-frequency QPO (HFQPO) at 67 Hz has been observed in this source, albeit less often than the type-C QPOs. Besides these features, GRS 1915+105 sometimes shows a broad bump in the power spectrum at around 30-150 Hz. We study the power spectra of GRS 1915+105 with the Rossi X-ray Timing Explorer when the source was in the χ class. We find that the rms amplitude of the bump depends strongly upon both the frequency of the type-C QPO and the hardness ratio, and is correlated with the corona temperature and anticorrelated with the radio flux at 15 GHz. The characteristic frequency of the bump is better correlated with a combination of the frequency of the type-C QPO and the hardness ratio than with the frequency of the type-C QPO alone. The rms amplitude of the bump generally increases with energy from ∼1-2 per cent at ∼3 keV to ∼10-15 per cent at ∼30 keV. We suggest that the bump and the HFQPO may be the same variability component but the properties of the corona affect the coherence of this variability, leading either to a HFQPO when the spectrum is in the relatively soft γclass, or to a bump when the spectrum is in the hard χ class. Finally, we discuss the anticorrelation between the rms amplitude of the bump and the radio flux in the context of the relation between the corona and the jet.
Fil: Zhang, Yuexin. University of Groningen; Países Bajos
Fil: Mendez, Raul Mariano. University of Groningen; Países Bajos. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
Fil: García, Federico. University of Groningen; Países Bajos. 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
Fil: Karpouzas, Konstantinos. University of Southampton; Reino Unido
Fil: Zhang, Liang. University of Southampton; Reino Unido
Fil: Liu, Honghui. Fudan University; China
Fil: Belloni, Tomaso M.. No especifíca;
Fil: Altamirano, Diego. University of Southampton; Reino Unido
description GRS 1915+105 can show type-C quasi-periodic oscillations (QPOs) in the power density spectrum. A high-frequency QPO (HFQPO) at 67 Hz has been observed in this source, albeit less often than the type-C QPOs. Besides these features, GRS 1915+105 sometimes shows a broad bump in the power spectrum at around 30-150 Hz. We study the power spectra of GRS 1915+105 with the Rossi X-ray Timing Explorer when the source was in the χ class. We find that the rms amplitude of the bump depends strongly upon both the frequency of the type-C QPO and the hardness ratio, and is correlated with the corona temperature and anticorrelated with the radio flux at 15 GHz. The characteristic frequency of the bump is better correlated with a combination of the frequency of the type-C QPO and the hardness ratio than with the frequency of the type-C QPO alone. The rms amplitude of the bump generally increases with energy from ∼1-2 per cent at ∼3 keV to ∼10-15 per cent at ∼30 keV. We suggest that the bump and the HFQPO may be the same variability component but the properties of the corona affect the coherence of this variability, leading either to a HFQPO when the spectrum is in the relatively soft γclass, or to a bump when the spectrum is in the hard χ class. Finally, we discuss the anticorrelation between the rms amplitude of the bump and the radio flux in the context of the relation between the corona and the jet.
publishDate 2022
dc.date.none.fl_str_mv 2022-08
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/11336/216794
Zhang, Yuexin; Mendez, Raul Mariano; García, Federico; Karpouzas, Konstantinos; Zhang, Liang; et al.; The evolution of the high-frequency variability in the black hole candidate GRS 1915+105 as seen by RXTE; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 514; 2; 8-2022; 2891-2901
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/216794
identifier_str_mv Zhang, Yuexin; Mendez, Raul Mariano; García, Federico; Karpouzas, Konstantinos; Zhang, Liang; et al.; The evolution of the high-frequency variability in the black hole candidate GRS 1915+105 as seen by RXTE; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 514; 2; 8-2022; 2891-2901
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/stac1050
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
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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