Show simple item record

dc.contributor.authorEsin, Ann A.
dc.contributor.authorMcClintock, Jeffrey E.
dc.contributor.authorNarayan, Ramesh
dc.date.accessioned2019-09-22T14:24:13Z
dc.date.issued1997
dc.identifier.citationEsin, Ann A., Jeffrey E. McClintock, and Ramesh Narayan. 1997. “Advection‐Dominated Accretion and the Spectral States of Black Hole X‐Ray Binaries: Application to Nova Muscae 1991.” The Astrophysical Journal 489 (2): 865–89. https://doi.org/10.1086/304829.
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.urihttp://nrs.harvard.edu/urn-3:HUL.InstRepos:41384907*
dc.description.abstractBlack hole X-ray binaries (BHXBs) are known to display five distinct spectral states. In order of increasing luminosity these are the quiescent state, low state, intermediate state, high state, and very high state. We present a self-consistent model of accretion flows around black holes that unifies all of these states except the very high state. The model is an extension of the following paradigm, which has been applied successfully to the quiescent state. The accretion flow consists of two zones, an inner advection-dominated accretion flow (ADAF) that extends from the black hole horizon to a transition radius r(tr), and an outer thin accretion disk that is present beyond r(tr). Above the disk is a hot corona, which is a continuation of the inner ADAF. The model consistently treats the dynamics of the accreting gas, the thermal balance of the ions and electrons in the two-temperature ADAF and corona, and the radiation processes that produce the observed spectrum.At low mass accretion rates, (m) over dot less than or similar to 0.01 (in Eddington units), the inner ADAF zone in the model radiates extremely inefficiently, and the outer thin disk is restricted to large radii (r(tr) similar to 10(2)-10(4), in Schwarzschild units). The luminosity therefore is low, and this configuration is identified with the quiescent state. For (m) over dot greater than or similar to 0.01 and up to a critical value (m) over dot(crit) similar to 0.08, the radiative efficiency of the ADAF increases rapidly and the system becomes fairly luminous. The spectrum is very hard and peaks around 100 keV. This is the low state. The exact value of (m) over dot(crit) depends on the viscosity parameter alpha ((m) over dot(crit) similar to 1.3 alpha(2); the paper assumes alpha = 0.25). For values of (m) over dot > (m) over dot(crit) and up to a second critical value about 10% higher, the ADAF progressively shrinks in size, the transition radius decreases, and the X-ray spectrum changes continuously from hard to soft. We identify this stage with the intermediate state. Finally, when (m) over dot is sufficiently large, the inner ADAF zone disappears altogether and the thin accretion disk extends down to the marginally stable orbit. The spectrum is dominated by an ultrasoft component with a weak hard tail. This is the high state. Model spectra calculated with this unified scenario agree well with observations of the quiescent, low, intermediate, and high states. Moreover, the model provides a natural explanation for the low state to high state transition in BHXBs. We also make a tentative proposal for the very high state, but this aspect of the model is less secure.An important feature of the model is that it is essentially parameter free. We test the model against observations of the soft X-ray transient Nova Muscae during its 1991 outburst. The model reproduces the observed light curves and spectra surprisingly well and makes a number of predictions that can be tested by observations of other BHXBs.
dc.language.isoen_US
dc.publisherAmerican Astronomical Society
dash.licenseLAA
dc.titleAdvection‐Dominated Accretion and the Spectral States of Black Hole X‐Ray Binaries: Application to Nova Muscae 1991
dc.typeJournal Article
dc.description.versionAccepted Manuscript
dc.relation.journalThe Astrophysical Journal
dash.depositing.authorNarayan, Ramesh::dc7afe5d74d62c7b451015317ea2ccbe::600
dc.date.available2019-09-22T14:24:13Z
dash.workflow.comments1Science Serial ID 95167
dc.identifier.doi10.1086/304829
dash.source.volume489;2
dash.source.page865-889


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record