A systematic study of the high-frequency bump in the black-hole low-mass X-ray binary GX 339 -4

Autores
Zhang, Yuexin; Méndez, Mariano; Motta, Sara E.; Zdziarski, Andrzej A.; Marcel, Grégoire; García, Federico; Altamirano, Diego; Belloni, Tomaso M.; Zhang, Liang; Timmermans, Thimo; Zhang, Guobao
Año de publicación
2024
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
The high-frequency bump, characterized by a frequency exceeding ∼30 Hz, represents a seldom-explored time-variability feature in the power density spectrum (PDS) of black-hole X-ray binaries. In the 2002, 2004, 2007, and 2010 outbursts of GX 339 -4, the bump has been occasionally observed in conjunction with type-C quasi-periodic oscillations (QPOs). We systematically study the properties of the bump during these four outbursts observed by Rossi X-ray Timing Explorer ( RXTE ) in the 2-60 keV bands and detect the bump in 39 observations. While the frequencies of the type-C QPOs are in the range of ∼0.1-9 Hz, the root-mean-square (rms) amplitude of the bump shows an evolution in the hardness ratio versus the type-C QPO frequency plot. By comparing the rms amplitude of the bump with the corona temperature and simultaneous radio jet flux of the source, as previously studied in GRS 1915 + 105, we establish that in the hard state of GX 339 -4, the bump is al w ays strong, with the measurements of the rms amplitude in the range of 4-10 per cent. At the same time, the corona temperature is high and the radio flux is low. These findings indicate that, using the bump as a proxy, the majority of the accretion energy is directed towards the hot corona rather than being channeled into the radio jet. We discuss this phenomenon in terms of an inefficient energy transfer mechanism between the corona and jet in GX 339 -4.
Fil: Zhang, Yuexin. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Méndez, Mariano. University of Groningen; Países Bajos
Fil: Motta, Sara E.. Osservatorio Astronomico Di Brera; Italia
Fil: Zdziarski, Andrzej A.. Polish Academy of Sciences; Polonia
Fil: Marcel, Grégoire. University of Cambridge; Reino Unido
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
Fil: Altamirano, Diego. University of Southampton; Reino Unido
Fil: Belloni, Tomaso M.. Osservatorio Astronomico Di Brera; Italia
Fil: Zhang, Liang. Chinese Academy of Sciences; República de China
Fil: Timmermans, Thimo. University of Groningen; Países Bajos
Fil: Zhang, Guobao. Chinese Academy of Sciences; República de China
Materia
ACCRETION, ACCRETION DISCS
STARS: BLACK HOLES
STARS: INDIVIDUAL: GX 339 -4
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:11336/231205
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/231205
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling A systematic study of the high-frequency bump in the black-hole low-mass X-ray binary GX 339 -4Zhang, YuexinMéndez, MarianoMotta, Sara E.Zdziarski, Andrzej A.Marcel, GrégoireGarcía, FedericoAltamirano, DiegoBelloni, Tomaso M.Zhang, LiangTimmermans, ThimoZhang, GuobaoACCRETION, ACCRETION DISCSSTARS: BLACK HOLESSTARS: INDIVIDUAL: GX 339 -4X-RAYS: BINARIEShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The high-frequency bump, characterized by a frequency exceeding ∼30 Hz, represents a seldom-explored time-variability feature in the power density spectrum (PDS) of black-hole X-ray binaries. In the 2002, 2004, 2007, and 2010 outbursts of GX 339 -4, the bump has been occasionally observed in conjunction with type-C quasi-periodic oscillations (QPOs). We systematically study the properties of the bump during these four outbursts observed by Rossi X-ray Timing Explorer ( RXTE ) in the 2-60 keV bands and detect the bump in 39 observations. While the frequencies of the type-C QPOs are in the range of ∼0.1-9 Hz, the root-mean-square (rms) amplitude of the bump shows an evolution in the hardness ratio versus the type-C QPO frequency plot. By comparing the rms amplitude of the bump with the corona temperature and simultaneous radio jet flux of the source, as previously studied in GRS 1915 + 105, we establish that in the hard state of GX 339 -4, the bump is al w ays strong, with the measurements of the rms amplitude in the range of 4-10 per cent. At the same time, the corona temperature is high and the radio flux is low. These findings indicate that, using the bump as a proxy, the majority of the accretion energy is directed towards the hot corona rather than being channeled into the radio jet. We discuss this phenomenon in terms of an inefficient energy transfer mechanism between the corona and jet in GX 339 -4.Fil: Zhang, Yuexin. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Méndez, Mariano. University of Groningen; Países BajosFil: Motta, Sara E.. Osservatorio Astronomico Di Brera; ItaliaFil: Zdziarski, Andrzej A.. Polish Academy of Sciences; PoloniaFil: Marcel, Grégoire. University of Cambridge; Reino UnidoFil: 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; ArgentinaFil: Altamirano, Diego. University of Southampton; Reino UnidoFil: Belloni, Tomaso M.. Osservatorio Astronomico Di Brera; ItaliaFil: Zhang, Liang. Chinese Academy of Sciences; República de ChinaFil: Timmermans, Thimo. University of Groningen; Países BajosFil: Zhang, Guobao. Chinese Academy of Sciences; República de ChinaWiley Blackwell Publishing, Inc2024-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/231205Zhang, Yuexin; Méndez, Mariano; Motta, Sara E.; Zdziarski, Andrzej A.; Marcel, Grégoire; et al.; A systematic study of the high-frequency bump in the black-hole low-mass X-ray binary GX 339 -4; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 527; 3; 1-2024; 5638-56480035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stad3623info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/527/3/5638/7450465info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:53:47Zoai:ri.conicet.gov.ar:11336/231205instacron: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 11:53:47.588CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv A systematic study of the high-frequency bump in the black-hole low-mass X-ray binary GX 339 -4
title A systematic study of the high-frequency bump in the black-hole low-mass X-ray binary GX 339 -4
spellingShingle A systematic study of the high-frequency bump in the black-hole low-mass X-ray binary GX 339 -4
Zhang, Yuexin
ACCRETION, ACCRETION DISCS
STARS: BLACK HOLES
STARS: INDIVIDUAL: GX 339 -4
X-RAYS: BINARIES
title_short A systematic study of the high-frequency bump in the black-hole low-mass X-ray binary GX 339 -4
title_full A systematic study of the high-frequency bump in the black-hole low-mass X-ray binary GX 339 -4
title_fullStr A systematic study of the high-frequency bump in the black-hole low-mass X-ray binary GX 339 -4
title_full_unstemmed A systematic study of the high-frequency bump in the black-hole low-mass X-ray binary GX 339 -4
title_sort A systematic study of the high-frequency bump in the black-hole low-mass X-ray binary GX 339 -4
dc.creator.none.fl_str_mv Zhang, Yuexin
Méndez, Mariano
Motta, Sara E.
Zdziarski, Andrzej A.
Marcel, Grégoire
García, Federico
Altamirano, Diego
Belloni, Tomaso M.
Zhang, Liang
Timmermans, Thimo
Zhang, Guobao
author Zhang, Yuexin
author_facet Zhang, Yuexin
Méndez, Mariano
Motta, Sara E.
Zdziarski, Andrzej A.
Marcel, Grégoire
García, Federico
Altamirano, Diego
Belloni, Tomaso M.
Zhang, Liang
Timmermans, Thimo
Zhang, Guobao
author_role author
author2 Méndez, Mariano
Motta, Sara E.
Zdziarski, Andrzej A.
Marcel, Grégoire
García, Federico
Altamirano, Diego
Belloni, Tomaso M.
Zhang, Liang
Timmermans, Thimo
Zhang, Guobao
author2_role author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv ACCRETION, ACCRETION DISCS
STARS: BLACK HOLES
STARS: INDIVIDUAL: GX 339 -4
X-RAYS: BINARIES
topic ACCRETION, ACCRETION DISCS
STARS: BLACK HOLES
STARS: INDIVIDUAL: GX 339 -4
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 high-frequency bump, characterized by a frequency exceeding ∼30 Hz, represents a seldom-explored time-variability feature in the power density spectrum (PDS) of black-hole X-ray binaries. In the 2002, 2004, 2007, and 2010 outbursts of GX 339 -4, the bump has been occasionally observed in conjunction with type-C quasi-periodic oscillations (QPOs). We systematically study the properties of the bump during these four outbursts observed by Rossi X-ray Timing Explorer ( RXTE ) in the 2-60 keV bands and detect the bump in 39 observations. While the frequencies of the type-C QPOs are in the range of ∼0.1-9 Hz, the root-mean-square (rms) amplitude of the bump shows an evolution in the hardness ratio versus the type-C QPO frequency plot. By comparing the rms amplitude of the bump with the corona temperature and simultaneous radio jet flux of the source, as previously studied in GRS 1915 + 105, we establish that in the hard state of GX 339 -4, the bump is al w ays strong, with the measurements of the rms amplitude in the range of 4-10 per cent. At the same time, the corona temperature is high and the radio flux is low. These findings indicate that, using the bump as a proxy, the majority of the accretion energy is directed towards the hot corona rather than being channeled into the radio jet. We discuss this phenomenon in terms of an inefficient energy transfer mechanism between the corona and jet in GX 339 -4.
Fil: Zhang, Yuexin. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Méndez, Mariano. University of Groningen; Países Bajos
Fil: Motta, Sara E.. Osservatorio Astronomico Di Brera; Italia
Fil: Zdziarski, Andrzej A.. Polish Academy of Sciences; Polonia
Fil: Marcel, Grégoire. University of Cambridge; Reino Unido
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
Fil: Altamirano, Diego. University of Southampton; Reino Unido
Fil: Belloni, Tomaso M.. Osservatorio Astronomico Di Brera; Italia
Fil: Zhang, Liang. Chinese Academy of Sciences; República de China
Fil: Timmermans, Thimo. University of Groningen; Países Bajos
Fil: Zhang, Guobao. Chinese Academy of Sciences; República de China
description The high-frequency bump, characterized by a frequency exceeding ∼30 Hz, represents a seldom-explored time-variability feature in the power density spectrum (PDS) of black-hole X-ray binaries. In the 2002, 2004, 2007, and 2010 outbursts of GX 339 -4, the bump has been occasionally observed in conjunction with type-C quasi-periodic oscillations (QPOs). We systematically study the properties of the bump during these four outbursts observed by Rossi X-ray Timing Explorer ( RXTE ) in the 2-60 keV bands and detect the bump in 39 observations. While the frequencies of the type-C QPOs are in the range of ∼0.1-9 Hz, the root-mean-square (rms) amplitude of the bump shows an evolution in the hardness ratio versus the type-C QPO frequency plot. By comparing the rms amplitude of the bump with the corona temperature and simultaneous radio jet flux of the source, as previously studied in GRS 1915 + 105, we establish that in the hard state of GX 339 -4, the bump is al w ays strong, with the measurements of the rms amplitude in the range of 4-10 per cent. At the same time, the corona temperature is high and the radio flux is low. These findings indicate that, using the bump as a proxy, the majority of the accretion energy is directed towards the hot corona rather than being channeled into the radio jet. We discuss this phenomenon in terms of an inefficient energy transfer mechanism between the corona and jet in GX 339 -4.
publishDate 2024
dc.date.none.fl_str_mv 2024-01
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/11336/231205
Zhang, Yuexin; Méndez, Mariano; Motta, Sara E.; Zdziarski, Andrzej A.; Marcel, Grégoire; et al.; A systematic study of the high-frequency bump in the black-hole low-mass X-ray binary GX 339 -4; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 527; 3; 1-2024; 5638-5648
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/231205
identifier_str_mv Zhang, Yuexin; Méndez, Mariano; Motta, Sara E.; Zdziarski, Andrzej A.; Marcel, Grégoire; et al.; A systematic study of the high-frequency bump in the black-hole low-mass X-ray binary GX 339 -4; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 527; 3; 1-2024; 5638-5648
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/stad3623
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/527/3/5638/7450465
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 12.982451

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