Time variability of low angular momentum accretion flows around black hole. (arXiv:1912.01418v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Palit_I/0/1/0/all/0/1">Ishika Palit</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Janiuk_A/0/1/0/all/0/1">Agnieszka Janiuk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sukova_P/0/1/0/all/0/1">Petra Sukova</a>
We present the relativistic 2D and 3D GRMHD simulation of axisymmetric,
inviscid, hydrodynamic accretion flows in a fixed Kerr black hole gravitational
field. The flow is having low angular momentum with respect to Keplerian one. A
relativistic fluid where its bulk velocity is comparable to the speed of light,
flowing in the accretion disk very close to the horizon should be described by
adiabtic index: 4=3 < g < 5=3 .The time dependent evolution of shock position
and respective effect on mass accretion rate and oscillation frequency with
varying adiabatic index has been studied. Here we present some of the results
for adiabatic index = 1.4 in a 2D and 3D model.
We present the relativistic 2D and 3D GRMHD simulation of axisymmetric,
inviscid, hydrodynamic accretion flows in a fixed Kerr black hole gravitational
field. The flow is having low angular momentum with respect to Keplerian one. A
relativistic fluid where its bulk velocity is comparable to the speed of light,
flowing in the accretion disk very close to the horizon should be described by
adiabtic index: 4=3 < g < 5=3 .The time dependent evolution of shock position
and respective effect on mass accretion rate and oscillation frequency with
varying adiabatic index has been studied. Here we present some of the results
for adiabatic index = 1.4 in a 2D and 3D model.
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