AustralieFrV1, PascalFrancis, Corpus, bibRecord, 001C42

Radiatively efficient accreting black holes in the hard state: the case study of H1743-322

Identifieur interne : 001C42 ( PascalFrancis/Corpus ); précédent : 001C41; suivant : 001C43

Radiatively efficient accreting black holes in the hard state: the case study of H1743-322

Auteurs : M. Coriat ; S. Corbel ; L. Prat ; J. C. A. Miller-Jones ; D. Cseh ; A. K. Tzioumis ; C. Brocksopp ; J. Rodriguez ; R. P. Fender ; G. R. Sivakoff

Source :

Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011.

RBID : Pascal:11-0283166

Descripteurs français

Pascal (Inist)
- Trou noir, Etude cas, Accrétion, Jet, Objet compact, Corrélation, Masse stellaire, Emission radioélectrique, Luminosité, Emission RX, Binaire RX, Source RX binaire, Disque accrétion, Etoile radio, Continuum, Cosmologie, Source RX cosmique.

English descriptors

KwdEn :
- Accretion, Accretion disks, Binary X ray source, Black holes, Case study, Compact objects, Continuum, Correlations, Cosmic x-ray sources, Cosmology, Jets, Luminosity, Radio emission, Radio stars, Stellar mass, X ray emission, X-ray binary stars.

Abstract

In recent years, much effort has been devoted to unravelling the connection between the accretion flow and the jets in accreting compact objects. In the present work, we report new constraints on these issues, through the long-term study of the radio and X-ray behaviour of the black hole candidate H1743-322. This source is known to be one of the 'outliers' of the universal radio/X-ray correlation, i.e. a group of accreting stellar-mass black holes displaying fainter radio emission for a given X-ray luminosity than expected from the correlation. Our study shows that the radio and X-ray emission of H1743-322 are strongly correlated at high luminosity in the hard spectral state. However, this correlation is unusually steep for a black hole X-ray binary: b ˜ 1.4 (with L_radio L^b_X). Below a critical luminosity, the correlation becomes shallower until it rejoins the standard correlation with b ˜ 0.6. Based on these results, we first show that the steep correlation can be explained if the inner accretion flow is radiatively efficient during the hard state, in contrast to what is usually assumed for black hole X-ray binaries in this spectral state. The transition between the steep and the standard correlation would therefore reflect a change from a radiatively efficient to a radiatively inefficient accretion flow. Finally, we investigate the possibility that the discrepancy between 'outliers' and 'standard' black holes arises from the outflow properties rather than from the accretion flow.

Notice en format standard (ISO 2709)

Pour connaître la documentation sur le format Inist Standard.

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C01	`01`		`ENG`	@0 In recent years, much effort has been devoted to unravelling the connection between the accretion flow and the jets in accreting compact objects. In the present work, we report new constraints on these issues, through the long-term study of the radio and X-ray behaviour of the black hole candidate H1743-322. This source is known to be one of the 'outliers' of the universal radio/X-ray correlation, i.e. a group of accreting stellar-mass black holes displaying fainter radio emission for a given X-ray luminosity than expected from the correlation. Our study shows that the radio and X-ray emission of H1743-322 are strongly correlated at high luminosity in the hard spectral state. However, this correlation is unusually steep for a black hole X-ray binary: b ˜ 1.4 (with L_radio <is proportional to> L^b_X). Below a critical luminosity, the correlation becomes shallower until it rejoins the standard correlation with b ˜ 0.6. Based on these results, we first show that the steep correlation can be explained if the inner accretion flow is radiatively efficient during the hard state, in contrast to what is usually assumed for black hole X-ray binaries in this spectral state. The transition between the steep and the standard correlation would therefore reflect a change from a radiatively efficient to a radiatively inefficient accretion flow. Finally, we investigate the possibility that the discrepancy between 'outliers' and 'standard' black holes arises from the outflow properties rather than from the accretion flow.
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Format Inist (serveur)

NO :	PASCAL 11-0283166 INIST
ET :	Radiatively efficient accreting black holes in the hard state: the case study of H1743-322
AU :	CORIAT (M.); CORBEL (S.); PRAT (L.); MILLER-JONES (J. C. A.); CSEH (D.); TZIOUMIS (A. K.); BROCKSOPP (C.); RODRIGUEZ (J.); FENDER (R. P.); SIVAKOFF (G. R.)
AF :	Laboraloire AIM, CEA-IRFU/CNRS/Université Paris Diderot, CEA Saclay/91191 Gif-sur-Yvette/France (1 aut., 2 aut., 3 aut., 5 aut., 8 aut.); Institut Universitaire de France/75005 Paris/France (2 aut.); NRAO Headquarters, 520 Edgemont Road/Charlottesville, VA 22903/Etats-Unis (4 aut.); International Centre for Radio Astronomy Research - Curtin University, GPO Box U1987/Perth, WA 6845/Australie (4 aut.); Australia Telescope National Facility, CSIRO, PO Box 76/Epping, NSW 1710/Australie (6 aut.); Mullard Space Science Laboratory, University College London, Holmbury St. Mary/Dorking, Surrey RH5 6NT/Royaume-Uni (7 aut.); School of Physics and Astronomy, University of Southampton/Highfield, Southampton SO17 1BJ/Royaume-Uni (9 aut.); Department of Astronomy, University of Virgina, PO Box 400325/Charlottesville, VA 22904-4325/Etats-Unis (10 aut.)
DT :	Publication en série; Niveau analytique
SO :	Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Etats-Unis; Da. 2011; Vol. 414; No. 1; Pp. 677-690; Bibl. 1 p.1/4
LA :	Anglais
EA :	In recent years, much effort has been devoted to unravelling the connection between the accretion flow and the jets in accreting compact objects. In the present work, we report new constraints on these issues, through the long-term study of the radio and X-ray behaviour of the black hole candidate H1743-322. This source is known to be one of the 'outliers' of the universal radio/X-ray correlation, i.e. a group of accreting stellar-mass black holes displaying fainter radio emission for a given X-ray luminosity than expected from the correlation. Our study shows that the radio and X-ray emission of H1743-322 are strongly correlated at high luminosity in the hard spectral state. However, this correlation is unusually steep for a black hole X-ray binary: b ˜ 1.4 (with L_radio <is proportional to> L^b_X). Below a critical luminosity, the correlation becomes shallower until it rejoins the standard correlation with b ˜ 0.6. Based on these results, we first show that the steep correlation can be explained if the inner accretion flow is radiatively efficient during the hard state, in contrast to what is usually assumed for black hole X-ray binaries in this spectral state. The transition between the steep and the standard correlation would therefore reflect a change from a radiatively efficient to a radiatively inefficient accretion flow. Finally, we investigate the possibility that the discrepancy between 'outliers' and 'standard' black holes arises from the outflow properties rather than from the accretion flow.
CC :	001E03
FD :	Trou noir; Etude cas; Accrétion; Jet; Objet compact; Corrélation; Masse stellaire; Emission radioélectrique; Luminosité; Emission RX; Binaire RX; Source RX binaire; Disque accrétion; Etoile radio; Continuum; Cosmologie; Source RX cosmique
ED :	Black holes; Case study; Accretion; Jets; Compact objects; Correlations; Stellar mass; Radio emission; Luminosity; X ray emission; X-ray binary stars; Binary X ray source; Accretion disks; Radio stars; Continuum; Cosmology; Cosmic x-ray sources
SD :	Estudio caso; Emisión radioeléctrica; Emisión RX; Fuente RX binaria; Continuo
LO :	INIST-2067.354000192158480530
ID :	11-0283166

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Pascal:11-0283166

Le document en format XML

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<sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Radiatively efficient accreting black holes in the hard state: the case study of H1743-322</title>
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<author><name sortKey="Cseh, D" sort="Cseh, D" uniqKey="Cseh D" first="D." last="Cseh">D. Cseh</name>
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<author><name sortKey="Tzioumis, A K" sort="Tzioumis, A K" uniqKey="Tzioumis A" first="A. K." last="Tzioumis">A. K. Tzioumis</name>
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<author><name sortKey="Brocksopp, C" sort="Brocksopp, C" uniqKey="Brocksopp C" first="C." last="Brocksopp">C. Brocksopp</name>
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<author><name sortKey="Rodriguez, J" sort="Rodriguez, J" uniqKey="Rodriguez J" first="J." last="Rodriguez">J. Rodriguez</name>
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<term>Continuum</term>
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<front><div type="abstract" xml:lang="en">In recent years, much effort has been devoted to unravelling the connection between the accretion flow and the jets in accreting compact objects. In the present work, we report new constraints on these issues, through the long-term study of the radio and X-ray behaviour of the black hole candidate H1743-322. This source is known to be one of the 'outliers' of the universal radio/X-ray correlation, i.e. a group of accreting stellar-mass black holes displaying fainter radio emission for a given X-ray luminosity than expected from the correlation. Our study shows that the radio and X-ray emission of H1743-322 are strongly correlated at high luminosity in the hard spectral state. However, this correlation is unusually steep for a black hole X-ray binary: b ˜ 1.4 (with L<sub>radio</sub>
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<sub>X</sub>
). Below a critical luminosity, the correlation becomes shallower until it rejoins the standard correlation with b ˜ 0.6. Based on these results, we first show that the steep correlation can be explained if the inner accretion flow is radiatively efficient during the hard state, in contrast to what is usually assumed for black hole X-ray binaries in this spectral state. The transition between the steep and the standard correlation would therefore reflect a change from a radiatively efficient to a radiatively inefficient accretion flow. Finally, we investigate the possibility that the discrepancy between 'outliers' and 'standard' black holes arises from the outflow properties rather than from the accretion flow.</div>
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<sub>X</sub>
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<ET>Radiatively efficient accreting black holes in the hard state: the case study of H1743-322</ET>
<AU>CORIAT (M.); CORBEL (S.); PRAT (L.); MILLER-JONES (J. C. A.); CSEH (D.); TZIOUMIS (A. K.); BROCKSOPP (C.); RODRIGUEZ (J.); FENDER (R. P.); SIVAKOFF (G. R.)</AU>
<AF>Laboraloire AIM, CEA-IRFU/CNRS/Université Paris Diderot, CEA Saclay/91191 Gif-sur-Yvette/France (1 aut., 2 aut., 3 aut., 5 aut., 8 aut.); Institut Universitaire de France/75005 Paris/France (2 aut.); NRAO Headquarters, 520 Edgemont Road/Charlottesville, VA 22903/Etats-Unis (4 aut.); International Centre for Radio Astronomy Research - Curtin University, GPO Box U1987/Perth, WA 6845/Australie (4 aut.); Australia Telescope National Facility, CSIRO, PO Box 76/Epping, NSW 1710/Australie (6 aut.); Mullard Space Science Laboratory, University College London, Holmbury St. Mary/Dorking, Surrey RH5 6NT/Royaume-Uni (7 aut.); School of Physics and Astronomy, University of Southampton/Highfield, Southampton SO17 1BJ/Royaume-Uni (9 aut.); Department of Astronomy, University of Virgina, PO Box 400325/Charlottesville, VA 22904-4325/Etats-Unis (10 aut.)</AF>
<DT>Publication en série; Niveau analytique</DT>
<SO>Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Etats-Unis; Da. 2011; Vol. 414; No. 1; Pp. 677-690; Bibl. 1 p.1/4</SO>
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<EA>In recent years, much effort has been devoted to unravelling the connection between the accretion flow and the jets in accreting compact objects. In the present work, we report new constraints on these issues, through the long-term study of the radio and X-ray behaviour of the black hole candidate H1743-322. This source is known to be one of the 'outliers' of the universal radio/X-ray correlation, i.e. a group of accreting stellar-mass black holes displaying fainter radio emission for a given X-ray luminosity than expected from the correlation. Our study shows that the radio and X-ray emission of H1743-322 are strongly correlated at high luminosity in the hard spectral state. However, this correlation is unusually steep for a black hole X-ray binary: b ˜ 1.4 (with L<sub>radio</sub>
  L<sup>b</sup>
<sub>X</sub>
). Below a critical luminosity, the correlation becomes shallower until it rejoins the standard correlation with b ˜ 0.6. Based on these results, we first show that the steep correlation can be explained if the inner accretion flow is radiatively efficient during the hard state, in contrast to what is usually assumed for black hole X-ray binaries in this spectral state. The transition between the steep and the standard correlation would therefore reflect a change from a radiatively efficient to a radiatively inefficient accretion flow. Finally, we investigate the possibility that the discrepancy between 'outliers' and 'standard' black holes arises from the outflow properties rather than from the accretion flow.</EA>
<CC>001E03</CC>
<FD>Trou noir; Etude cas; Accrétion; Jet; Objet compact; Corrélation; Masse stellaire; Emission radioélectrique; Luminosité; Emission RX; Binaire RX; Source RX binaire; Disque accrétion; Etoile radio; Continuum; Cosmologie; Source RX cosmique</FD>
<ED>Black holes; Case study; Accretion; Jets; Compact objects; Correlations; Stellar mass; Radio emission; Luminosity; X ray emission; X-ray binary stars; Binary X ray source; Accretion disks; Radio stars; Continuum; Cosmology; Cosmic x-ray sources</ED>
<SD>Estudio caso; Emisión radioeléctrica; Emisión RX; Fuente RX binaria; Continuo</SD>
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Radiatively efficient accreting black holes in the hard state: the case study of H1743-322

Radiatively efficient accreting black holes in the hard state: the case study of H1743-322

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