2015
DOI: 10.1093/mnras/stv223
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Segregation of a Keplerian disc and sub-Keplerian halo from a transonic flow around a black hole by viscosity and cooling processes

Abstract: A black hole accretion is necessarily transonic. In presence of sufficiently high viscosity and cooling effects, a low-angular momentum transonic flow can become a standard Keplerian disc except close to the where hole where it must pass through the inner sonic point. However, if the viscosity is not high everywhere and cooling is not efficient everywhere, the flow cannot completely become a Keplerian disc. In this paper, we show results of rigorous numerical simulations of a transonic flow having vertically v… Show more

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Cited by 27 publications
(10 citation statements)
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“…Indeed, we find that the accretion is very very low and almost all the matter is ejected as winds, often partially evacuating the disk itself when the outflow rate is higher than the inflow rate. In a realistic and generalized accretion process scenario on a black hole, one often finds signatures of two components where the viscous accretion disks are surrounded by low-angular momentum flows such as those we used in this paper (Chakrabarti 1996b;Giri & Chakrabarti 2013;Giri et al 2015;Chakrabarti et al 2015). In future, our goal would be to introduce viscosity and radiative processes to produce self-consistent spectrum out of disks around a rotating black hole.…”
Section: Discussionmentioning
confidence: 98%
“…Indeed, we find that the accretion is very very low and almost all the matter is ejected as winds, often partially evacuating the disk itself when the outflow rate is higher than the inflow rate. In a realistic and generalized accretion process scenario on a black hole, one often finds signatures of two components where the viscous accretion disks are surrounded by low-angular momentum flows such as those we used in this paper (Chakrabarti 1996b;Giri & Chakrabarti 2013;Giri et al 2015;Chakrabarti et al 2015). In future, our goal would be to introduce viscosity and radiative processes to produce self-consistent spectrum out of disks around a rotating black hole.…”
Section: Discussionmentioning
confidence: 98%
“…In a time independent model of CENBOL (following C85), this is not possible to show unless we carry out time dependent fluid dynamics results coupled with Monte-Carlo simulation which is very time consuming. The behavior of CENBOL in time dependent simulations are different than the thick disk geometry (for details see Molteni, Lanzafame, & Chakrabarti, 1994 (MLC94); Ryu, Chakrabarti, & Molteni, 1997 (RCM97), Giri & Chakrabarti et al 2010;Giri & Chakrabarti 2012;Giri, Garain & Chakrabarti 2015). The electron density inside Compton cloud is sharply high at the outer edge due to shock compression.…”
Section: Discussionmentioning
confidence: 99%
“…The Keplerian disk formation was seen through numerical simulations in one dimension 12 and in two dimensions. [13][14][15] In this case, centrifugal pressure supported shocks are produced first in the post-shock region where the shear stress is the highest (as the pressure is high) and then propagate outward while converting the sub-Keplerian flow into a Keplerian flow. Thus, if a low angular flow is injected into the system which becomes Keplerian only along the equatorial plane due to higher viscosity, the flow will be de-segregated into two components (CT95) and depending on the relative importance of the Keplerian rate with respect to the sub-Keplerian halo, the CEN-BOL may or may not be cooled down.…”
Section: Spectral State Transitionsmentioning
confidence: 99%
“…A Keplerian disk with certain accretion rate requires certain minimal stress to maintain itself. The Keplerian disk formation was seen through numerical simulations in one dimension 12 and in two dimensions [13][14][15] . In this case, centrifugal pressure supported shocks are produced first in the postshock region where the shear stress is the highest (as the pressure is high) and then propagate outward while converting the sub-Keplerian flow into a Keplerian flow.…”
Section: Spectral State Transitionsmentioning
confidence: 99%