Choked accretion onto a Kerr black hole. (arXiv:2009.06653v2 [astro-ph.HE] UPDATED)

Choked accretion onto a Kerr black hole. (arXiv:2009.06653v2 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Aguayo_Ortiz_A/0/1/0/all/0/1">Alejandro Aguayo-Ortiz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sarbach_O/0/1/0/all/0/1">Olivier Sarbach</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tejeda_E/0/1/0/all/0/1">Emilio Tejeda</a>

The choked accretion model consists of a purely hydrodynamical mechanism in
which, by setting an equatorial to polar density contrast, a spherically
symmetric accretion flow transitions to an inflow-outflow configuration. This
scenario has been studied in the case of a (non-rotating) Schwarzschild black
hole as central accretor, as well as in the non-relativistic limit. In this
article, we generalize these previous works by studying the accretion of a
perfect fluid onto a (rotating) Kerr black hole. We first describe the
mechanism by using a steady-state, irrotational analytic solution of an
ultrarelativistic perfect fluid, obeying a stiff equation of state. We then use
hydrodynamical numerical simulations in order to explore a more general
equation of state. Analyzing the effects of the black hole’s rotation on the
flow, we find in particular that the choked accretion inflow-outflow morphology
prevails for all possible values of the black hole’s spin parameter, showing
the robustness of the model.

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