Radiatively efficient accreting black holes in the hard state: the case study of H1743–322
Identifieur interne : 006342 ( Main/Exploration ); précédent : 006341; suivant : 006343Radiatively efficient accreting black holes in the hard state: the case study of H1743–322
Auteurs : M. Coriat [France, Royaume-Uni] ; S. Corbel [France] ; L. Prat [France] ; J. C. A. Miller-Jones [États-Unis, Australie] ; D. Cseh [France] ; A. K. Tzioumis [Australie] ; C. Brocksopp [Royaume-Uni] ; J. Rodriguez [France] ; R. P. Fender ; G. R. Sivakoff [États-Unis]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011-06-11.
Descripteurs français
- Pascal (Inist)
- Wicri :
- topic : Cosmologie.
English descriptors
- KwdEn :
- Accretion, Accretion disc, Accretion disks, Accretion rate, Accretion rates, Adaf, Astron, Atca, Australia telescope, Belloni, Bhxbs, Binary, Binary X ray source, Black hole, Black hole binaries, Black holes, Blandford, Cambridge univ, Case study, Chandra, Compact jets, Compact objects, Continuum, Corbel, Coriat, Corona, Correlation, Correlation index, Correlations, Cosmic x-ray sources, Cosmology, Count rate, Critical accretion rate, Dhawan, Fainter radio emission, Falcke, February, Fender, Ferreira, Galactic, Gallo, Hard state, High luminosity, Homan, Intermediate state, Island state, Jets, Jonker, Ledd, Lhaf, Lhaf regime, Light curve, Lradio, Lstand, Ltrans, Luminosity, Luminosity range, Markoff, Mass accretion rate, Mcclintock, Merloni, Migliari, Migliari fender, Mioduszewski, Mnras, Monthly notices, Neutron, Neutron star, Neutron star binaries, Normalization, Nowak, Outburst, Outlier, Photon, Photon index, Precise measurement, Quenching factor, Radiatively, Radiatively accretion, Radio emission, Radio luminosity, Radio observations, Radio stars, Radio wavelengths, Rding, Ridge emission, Rodriguez, Rupen, Rxte, Soft state, Spectral index, Standard correlation, Steep correlation, Stellar mass, Sunyaev, Synchrotron, Synchrotron emission, Thin synchrotron emission, Unabsorbed, Upper limit, Uxes, X ray emission, X-ray binary stars, Yuan.
- Teeft :
- Accretion, Accretion disc, Accretion rate, Accretion rates, Adaf, Astron, Atca, Australia telescope, Belloni, Bhxbs, Binary, Black hole, Black hole binaries, Black holes, Blandford, Cambridge univ, Chandra, Compact jets, Corbel, Coriat, Corona, Correlation, Correlation index, Count rate, Critical accretion rate, Dhawan, Fainter radio emission, Falcke, February, Fender, Ferreira, Galactic, Gallo, Hard state, High luminosity, Homan, Intermediate state, Island state, Jonker, Ledd, Lhaf, Lhaf regime, Light curve, Lradio, Lstand, Ltrans, Luminosity, Luminosity range, Markoff, Mass accretion rate, Mcclintock, Merloni, Migliari, Migliari fender, Mioduszewski, Mnras, Monthly notices, Neutron, Neutron star, Neutron star binaries, Normalization, Nowak, Outburst, Outlier, Photon, Photon index, Precise measurement, Quenching factor, Radiatively, Radiatively accretion, Radio emission, Radio luminosity, Radio observations, Radio wavelengths, Rding, Ridge emission, Rodriguez, Rupen, Rxte, Soft state, Spectral index, Standard correlation, Steep correlation, Sunyaev, Synchrotron, Synchrotron emission, Thin synchrotron emission, Unabsorbed, Upper limit, Uxes, Yuan.
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 Lradio∝LbX). 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.
Url:
DOI: 10.1111/j.1365-2966.2011.18433.x
Affiliations:
- Australie, France, Royaume-Uni, États-Unis
- Angleterre, Grand Londres, Virginie, Île-de-France
- Gif‐sur‐Yvette, Londres, Paris
- University College de Londres
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Le document en format XML
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Sivakoff</name><affiliation wicri:level="2"><country xml:lang="fr">États-Unis</country><wicri:regionArea>Department of Astronomy, University of Virgina, PO Box 400325, Charlottesville, VA 22904‐4325</wicri:regionArea><placeName><region type="state">Virginie</region></placeName></affiliation></author></analytic><monogr></monogr><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title><idno type="ISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><imprint><biblScope unit="vol">414</biblScope><biblScope unit="issue">1</biblScope><biblScope unit="page" from="677">677</biblScope><biblScope unit="page" to="690">690</biblScope><biblScope unit="page-count">14</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2011-06-11">2011-06-11</date></imprint><idno type="ISSN">0035-8711</idno></series></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Accretion</term><term>Accretion disc</term><term>Accretion disks</term><term>Accretion rate</term><term>Accretion rates</term><term>Adaf</term><term>Astron</term><term>Atca</term><term>Australia telescope</term><term>Belloni</term><term>Bhxbs</term><term>Binary</term><term>Binary X ray source</term><term>Black hole</term><term>Black hole binaries</term><term>Black holes</term><term>Blandford</term><term>Cambridge univ</term><term>Case study</term><term>Chandra</term><term>Compact jets</term><term>Compact objects</term><term>Continuum</term><term>Corbel</term><term>Coriat</term><term>Corona</term><term>Correlation</term><term>Correlation index</term><term>Correlations</term><term>Cosmic x-ray sources</term><term>Cosmology</term><term>Count rate</term><term>Critical accretion rate</term><term>Dhawan</term><term>Fainter radio emission</term><term>Falcke</term><term>February</term><term>Fender</term><term>Ferreira</term><term>Galactic</term><term>Gallo</term><term>Hard state</term><term>High luminosity</term><term>Homan</term><term>Intermediate state</term><term>Island state</term><term>Jets</term><term>Jonker</term><term>Ledd</term><term>Lhaf</term><term>Lhaf regime</term><term>Light curve</term><term>Lradio</term><term>Lstand</term><term>Ltrans</term><term>Luminosity</term><term>Luminosity range</term><term>Markoff</term><term>Mass accretion rate</term><term>Mcclintock</term><term>Merloni</term><term>Migliari</term><term>Migliari fender</term><term>Mioduszewski</term><term>Mnras</term><term>Monthly notices</term><term>Neutron</term><term>Neutron star</term><term>Neutron star binaries</term><term>Normalization</term><term>Nowak</term><term>Outburst</term><term>Outlier</term><term>Photon</term><term>Photon index</term><term>Precise measurement</term><term>Quenching factor</term><term>Radiatively</term><term>Radiatively accretion</term><term>Radio emission</term><term>Radio luminosity</term><term>Radio observations</term><term>Radio stars</term><term>Radio wavelengths</term><term>Rding</term><term>Ridge emission</term><term>Rodriguez</term><term>Rupen</term><term>Rxte</term><term>Soft state</term><term>Spectral index</term><term>Standard correlation</term><term>Steep correlation</term><term>Stellar mass</term><term>Sunyaev</term><term>Synchrotron</term><term>Synchrotron emission</term><term>Thin synchrotron emission</term><term>Unabsorbed</term><term>Upper limit</term><term>Uxes</term><term>X ray emission</term><term>X-ray binary stars</term><term>Yuan</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Accrétion</term><term>Binaire RX</term><term>Continuum</term><term>Corrélation</term><term>Cosmologie</term><term>Disque accrétion</term><term>Emission RX</term><term>Emission radioélectrique</term><term>Etoile radio</term><term>Etude cas</term><term>Jet</term><term>Luminosité</term><term>Masse stellaire</term><term>Objet compact</term><term>Source RX binaire</term><term>Source RX cosmique</term><term>Trou noir</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>Accretion</term><term>Accretion disc</term><term>Accretion rate</term><term>Accretion rates</term><term>Adaf</term><term>Astron</term><term>Atca</term><term>Australia telescope</term><term>Belloni</term><term>Bhxbs</term><term>Binary</term><term>Black hole</term><term>Black hole binaries</term><term>Black holes</term><term>Blandford</term><term>Cambridge univ</term><term>Chandra</term><term>Compact jets</term><term>Corbel</term><term>Coriat</term><term>Corona</term><term>Correlation</term><term>Correlation index</term><term>Count rate</term><term>Critical accretion rate</term><term>Dhawan</term><term>Fainter radio emission</term><term>Falcke</term><term>February</term><term>Fender</term><term>Ferreira</term><term>Galactic</term><term>Gallo</term><term>Hard state</term><term>High luminosity</term><term>Homan</term><term>Intermediate state</term><term>Island state</term><term>Jonker</term><term>Ledd</term><term>Lhaf</term><term>Lhaf regime</term><term>Light curve</term><term>Lradio</term><term>Lstand</term><term>Ltrans</term><term>Luminosity</term><term>Luminosity range</term><term>Markoff</term><term>Mass accretion rate</term><term>Mcclintock</term><term>Merloni</term><term>Migliari</term><term>Migliari fender</term><term>Mioduszewski</term><term>Mnras</term><term>Monthly notices</term><term>Neutron</term><term>Neutron star</term><term>Neutron star binaries</term><term>Normalization</term><term>Nowak</term><term>Outburst</term><term>Outlier</term><term>Photon</term><term>Photon index</term><term>Precise measurement</term><term>Quenching factor</term><term>Radiatively</term><term>Radiatively accretion</term><term>Radio emission</term><term>Radio luminosity</term><term>Radio observations</term><term>Radio wavelengths</term><term>Rding</term><term>Ridge emission</term><term>Rodriguez</term><term>Rupen</term><term>Rxte</term><term>Soft state</term><term>Spectral index</term><term>Standard correlation</term><term>Steep correlation</term><term>Sunyaev</term><term>Synchrotron</term><term>Synchrotron emission</term><term>Thin synchrotron emission</term><term>Unabsorbed</term><term>Upper limit</term><term>Uxes</term><term>Yuan</term></keywords><keywords scheme="Wicri" type="topic" xml:lang="fr"><term>Cosmologie</term></keywords></textClass></profileDesc></teiHeader><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 Lradio∝LbX). 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></front></TEI><affiliations><list><country><li>Australie</li><li>France</li><li>Royaume-Uni</li><li>États-Unis</li></country><region><li>Angleterre</li><li>Grand Londres</li><li>Virginie</li><li>Île-de-France</li></region><settlement><li>Gif‐sur‐Yvette</li><li>Londres</li><li>Paris</li></settlement><orgName><li>University College de Londres</li></orgName></list><tree><noCountry><name sortKey="Fender, R P" sort="Fender, R P" uniqKey="Fender R" first="R. P." last="Fender">R. P. Fender</name></noCountry><country name="France"><region name="Île-de-France"><name sortKey="Coriat, M" sort="Coriat, M" uniqKey="Coriat M" first="M." last="Coriat">M. Coriat</name></region><name sortKey="Corbel, S" sort="Corbel, S" uniqKey="Corbel S" first="S." last="Corbel">S. Corbel</name><name sortKey="Corbel, S" sort="Corbel, S" uniqKey="Corbel S" first="S." last="Corbel">S. Corbel</name><name sortKey="Cseh, D" sort="Cseh, D" uniqKey="Cseh D" first="D." last="Cseh">D. Cseh</name><name sortKey="Prat, L" sort="Prat, L" uniqKey="Prat L" first="L." last="Prat">L. Prat</name><name sortKey="Rodriguez, J" sort="Rodriguez, J" uniqKey="Rodriguez J" first="J." last="Rodriguez">J. Rodriguez</name></country><country name="Royaume-Uni"><noRegion><name sortKey="Coriat, M" sort="Coriat, M" uniqKey="Coriat M" first="M." last="Coriat">M. Coriat</name></noRegion><name sortKey="Brocksopp, C" sort="Brocksopp, C" uniqKey="Brocksopp C" first="C." last="Brocksopp">C. Brocksopp</name></country><country name="États-Unis"><region name="Virginie"><name sortKey="Miller Ones, J C A" sort="Miller Ones, J C A" uniqKey="Miller Ones J" first="J. C. A." last="Miller-Jones">J. C. A. 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