Shocks in the relativistic transonic accretion with low angular momentum

We performed 2D and 3D relativistic hydrodynamical simulations of accretion flows with low angular momentum, filling the gap between spherically symmetric Bondi accretion and disc-like accretion flows. Scenarios with different directional distributions of angular momentum of falling matter and varying values of key parameters such as spin of central black hole, energy and angular momentum of matter were considered. In some of the scenarios the shock front is formed. We identified the ranges of parameters for which the shock after formation moves towards or outwards the central black hole or the long lasting oscillating shock is observed. The frequencies of oscillations of shock positions which can cause flaring in mass accretion rate are extracted. The results are scalable with mass of central black hole and can be compared to the quasi-periodic oscillations of selected microquasars (such as GRS 1915+105, XTE J1550-564 or IGR J17091-3624), as well as to the supermassive black holes in the centers of weakly active galaxies, such as Sgr A*.

Our simulations with the full General Relativistic treatment are the first of this kind in the literature.

K500_NMRAS_122

Figure above presents the snapshot taken at time t=24,400 M (dynamical time units) of a 3-dimensional simulation of accretion onto a non-rotating black hole. The color maps present the distribution of quantities in the x-z plane: Mach number (top panel), density, and specific angular momentum (bottom panels). The solid line in middle panel shows the position of the inner and outer shock (M=1). In the time-dependent simulation, the position of shock fronts oscillates. (Author: Petra Sukova).


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