A two-temperature accretion disk model for Cygnus X-1 - Structure and spectrum

Shapiro, Stuart L.; Lightman, Alan P.; Eardley, Douglas M.

doi:10.1086/154162

Cited by 860 publications

(733 citation statements)

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“…An early suggestion [141] for the geometry of coronal systems was that the accretion disk consisted of two zones-a cool, outer disk, and a hot inner, disk. It was envisioned that energy release was actively occurring within the disk itself, but that a "two-temperature" disk was being formed within the inner regions.…”

Section: So Long As Ementioning

confidence: 99%

Fluorescent iron lines as a probe of astrophysical black hole systems

2003

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Section: So Long As Ementioning

confidence: 99%

Fluorescent iron lines as a probe of astrophysical black hole systems

2003

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“…If T e ∼ 10 9 K in the inner portion of the disk, a two-temperature solution is obtained (Shapiro, Lightman, andEardley, 1976: Eilek andKafatos, 1983), where the ions are much hotter than the electrons, T i ∼ 10 11 − 10 13 K. In such a disk, a puffed-up inner region is formed supported by the ion pressure. Unsaturated Comptonization transfers energy from the electrons to the soft photons emitted in the cooler, underlying disk.…”

Section: Two-temperature Disks and Ion-supported Torimentioning

confidence: 99%

“…Unsaturated Comptonization transfers energy from the electrons to the soft photons emitted in the cooler, underlying disk. The process is described by the dimensionless parameter y (Shapiro, Lightman, and Eardley, 1976), where y = ¡fractional energy change per scattering¿¡number of scatterings¿ or…”

Section: Two-temperature Disks and Ion-supported Torimentioning

confidence: 99%

“…Unsaturated Comptonization occurs for y ∼ 1 and is appropriate whenever there is a copious source of soft photons in the inner region (Shapiro, Lightman, and Eardley, 1976;Sunyaev and Titarchuk, 1985). The y-value is related to the energy flux spectral index A (where the energy flux is measured in keV cm − 2 s − 1 keV − 1) through A ∼ 0.72 y −0.917 (Kafatos, 1983) and as such y ∼ 1 provides a natural explanation for the spectra of many cosmic sources.…”

Section: Two-temperature Disks and Ion-supported Torimentioning

confidence: 99%

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Inner Region Accretion Flows Onto Black Holes

Kafatos¹,

Subramanian²

2001

The Neutron Star—Black Hole Connection

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We examine here the inner region accretion flows onto black holes. A variety of models are presented. We also discuss viscosity mechanisms under a variety of circumstances, for standard accretion disks onto galactic black holes and supermassive black holes and hot accretion disks. Relevant work is presented here on unified aspects of disk accretion onto supermassive black holes and the possible coupling of thick disks to beams in the inner regions. We also explore other accretion flow scenarios. We conclude that a variety of scenarios yield high temperatures in the inner flows and that viscosity is likely not higher than alpha ∼ 0.01.

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“…The standard opticly thick accretion disk (Shakura & Sunyaev 1973) breaks down at high accretion rate and, thus it puffs up producing the central, hot (∼100 keV) region (e.g. Shapiro, Lightman & Eardley 1976) which constitutes the Comptonizing X/γ source (e.g. Zdziarski et al 1997).…”

Section: Introductionmentioning

confidence: 99%

A Model of the Broad-Band Continuum of NGC 5548

Magdziarz

Blaes

1998

The Hot Universe

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Abstract. We discuss a model of the central source in Seyfert 1 galaxy NGC 5548. The model assumes a three phase disk structure consisting of a cold outer disk, a hot central disk constituting a Comptonizing X/γ source, and an intermediate unstable and complex phase emitting a soft excess component. The model qualitatively explains broad-band spectrum and variability behavior assuming that the soft excess contributes significantly to the continuum emission and drives variability by geometrical changes of the intermediate disk zone.

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A two-temperature accretion disk model for Cygnus X-1 - Structure and spectrum

Cited by 860 publications

References 0 publications

Fluorescent iron lines as a probe of astrophysical black hole systems

Fluorescent iron lines as a probe of astrophysical black hole systems

Inner Region Accretion Flows Onto Black Holes

A Model of the Broad-Band Continuum of NGC 5548

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