Thin accretion disk around the distorted Schwarzschild black hole. (arXiv:2010.02786v2 [astro-ph.HE] UPDATED)

<a href="http://arxiv.org/find/astro-ph/1/au:+Faraji_S/0/1/0/all/0/1">Shokoufe Faraji</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hackmann_E/0/1/0/all/0/1">Eva Hackmann</a>

We construct the relativistic standard steady, optically thick, cold and

geometrically thin accretion disk around a distorted Schwarzschild black hole.

The distortion of this static and axially symmetric black hole solution, is

connected to an external distribution of matter. If the effects due to the

rotation are negligible, this distribution can describe the exterior of any

axially symmetric astrophysical model. Also, the distortion could be related to

the outer parts of the accretion disk. We study the effects due to a distortion

up to the quadrupole, and compare the physical characteristics of this disk to

the usual Schwarzschild case.

We construct the relativistic standard steady, optically thick, cold and

geometrically thin accretion disk around a distorted Schwarzschild black hole.

The distortion of this static and axially symmetric black hole solution, is

connected to an external distribution of matter. If the effects due to the

rotation are negligible, this distribution can describe the exterior of any

axially symmetric astrophysical model. Also, the distortion could be related to

the outer parts of the accretion disk. We study the effects due to a distortion

up to the quadrupole, and compare the physical characteristics of this disk to

the usual Schwarzschild case.

http://arxiv.org/icons/sfx.gif