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

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.

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