Inertia of Heat in Advective Accretion Disks around Kerr Black Holes

Beloborodov, Andrei M.; Abramowicz, Marek A.; Новиков, И. Д.

doi:10.1086/304956

Cited by 11 publications

(12 citation statements)

References 8 publications

(14 reference statements)

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“…Another critical density for radial self-gravity, ðsg; rÞ, is 16ðsg; zÞ (Goldreich & Lynden-Bell 1965;see Huré 1998 for a review). The inertia of the heat (Beloborodov, Abramowicz, & Novikov 1997; dashed lines in the second panel) is always much smaller than the gas rest-mass density " in this study (disks around nonrotating BHs): rad a " T T 4 =c 2 ' 10 À11 ð " T T=10 6 KÞ 4 g cm À3 5 " (third panel). Finally, the effective temperature profiles T eff (r) before the relativistic correction (solid lines) are compared with those with the correction (dotted lines; eq.…”

Section: No 1 2003 Super-eddington Accretion Flow Of Bhsmentioning

confidence: 64%

Comptonization in Super‐Eddington Accretion Flow and Growth Timescale of Supermassive Black Holes

Kawaguchi

2003

ApJ

140

211

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Super-Eddington accretion onto black holes (BHs) may occur at ultraluminous compact X-ray sources in nearby galaxies, Galactic microquasars, and narrow-line Seyfert 1 galaxies (NLS1s). Effects of electron scattering (opacity and Comptonization) and the relativistic correction (gravitational redshift and transverse Doppler effect) on the emergent spectra from super-Eddington accretion flows onto nonrotating BHs are examined for 10 1.5 and 10 6.5 M BH masses (M BH ). With _ m m½ _ M M=ðL Edd =c 2 Þ ! 100 (where _ M M is the accretion rate), the spectral hardening factor via electron scattering is d2.3-6.5. As a result of the _ m m-sensitive hardening factor, the color temperature of the innermost radiation is not proportional to L 0.25 , differing from the simplest standard accretion disk. The model is applied to optical-soft X-ray emission from NLS1s. We pick up one NLS1, namely, PG 1448+273 with an inferred M BH of 10 6.4 M , among the highest _ m m candidates. The broadband spectral distribution is successfully reproduced by the model with an extremely high _ m m (=1000) and the viscosity parameter of 0.01. This implies that this object, as well as some other highest _ m m systems, is really young: the inferred age,, is about 10 6 yr. We also briefly discuss the distribution of _ m m for transient and highly variable NLS1s, finding that those are located at 3d _ m md300. Such a moderately high accretion rate is indicative of thermal instability. Furthermore, _ m m for a possible type 2 counterpart of NLS1s, NGC 1068, is found to be similar to _ m m for NLS1s.

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Section: No 1 2003 Super-eddington Accretion Flow Of Bhsmentioning

confidence: 64%

Comptonization in Super‐Eddington Accretion Flow and Growth Timescale of Supermassive Black Holes

Kawaguchi

2003

ApJ

140

211

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“…The rapid advection in ADAFs generally has two effects: 1) dissipated orbital energy can not be radiated locally before it is carried inward and 2) the rotation profile is generally no longer Keplerian, although Abramowicz [6] found solutions where the dominant cooling mechanism was advection, even when the angular momentum profile was Keplerian. Fully relativistic solutions of ADAFs have also been found numerically [13,41]. Further discussion of ADAFs is given in the review article by Narayan and McClintock [219].…”

Section: Advection-dominated Accretion Flows (Adafs)mentioning

confidence: 93%

Foundations of Black Hole Accretion Disk Theory

Abramowicz

Fragile

2013

Living Rev. Relativ.

569

488

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This review covers the main aspects of black hole accretion disk theory. We begin with the view that one of the main goals of the theory is to better understand the nature of black holes themselves. In this light we discuss how accretion disks might reveal some of the unique signatures of strong gravity: the event horizon, the innermost stable circular orbit, and the ergosphere. We then review, from a first-principles perspective, the physical processes at play in accretion disks. This leads us to the four primary accretion disk models that we review: Polish doughnuts (thick disks), Shakura-Sunyaev (thin) disks, slim disks, and advection-dominated accretion flows (ADAFs). After presenting the models we discuss issues of stability, oscillations, and jets. Following our review of the analytic work, we take a parallel approach in reviewing numerical studies of black hole accretion disks. We finish with a few select applications that highlight particular astrophysical applications: measurements of black hole mass and spin, black hole vs. neutron star accretion disks, black hole accretion disk spectral states, and quasi-periodic oscillations (QPOs).

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“…The main equations express the conservation laws for barion number, energy, angular momentum, and radial momentum. We include in the equations the inertial mass associated with internal energy accumulated in the flow (Beloborodov, Abramowicz & Novikov 1997).…”

Section: Relativistic Disc Equationsmentioning

confidence: 99%

Super-Eddington accretion discs around Kerr black holes

Beloborodov

1998

Monthly Notices of the Royal Astronomical Society

Self Cite

110

112

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We calculate the structure of the accretion disc around a rapidly rotating black hole with a super‐Eddington accretion rate. The luminosity and height of the disc are reduced by the advection effect. In the case of large viscosity parameter, α>0.03, the accretion flow deviates strongly from thermodynamic equilibrium and overheats in the central region. With increasing accretion rate, the flow temperature steeply increases, reaches maximum, and then falls off. The maximum is achieved in the advection‐dominated regime of accretion. The maximum temperature in the disc around a massive black hole of M=108 M⊙ with α=0.3 is of order 3×108 K. The discs with large accretion rates can emit X‐rays in quasars as well as in galactic black hole candidates.

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Inertia of Heat in Advective Accretion Disks around Kerr Black Holes

Cited by 11 publications

References 8 publications

Comptonization in Super‐Eddington Accretion Flow and Growth Timescale of Supermassive Black Holes

Comptonization in Super‐Eddington Accretion Flow and Growth Timescale of Supermassive Black Holes

Foundations of Black Hole Accretion Disk Theory

Super-Eddington accretion discs around Kerr black holes

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