Shocks in relativistic viscous accretion flows around Kerr black holes

Abstract

We study the relativistic viscous accretion flows around the Kerr black holes. We present the governing equations that describe the steady state flow motion in full general relativity and solve them in 1.5D to obtain the complete set of global transonic solutions in terms of the flow parameters, namely specific energy (E ), specific angular momentum (L ) and viscosity (α). We obtain a new type of accretion solution which was not reported earlier. Further, we show for the first time to the best of our knowledge that viscous accretion solutions may contain shock waves particularly when flow simultaneously passes through both inner critical point (r in ) and outer critical point (r out ) before entering into the Kerr black holes. We examine the shock properties, namely shock location (r s ) and compression ratio (R, the measure of density compression across the shock front) and show that shock can form for a large region of parameter space in L − E plane. We study the effect of viscous dissipation on the shock parameter space and find that parameter space shrinks as α is increased. We also calculate the critical viscosity parameter (α cri ) beyond which standing shock solutions disappear and examine the correlation between the black hole spin (a k ) and α cri . Finally, the relevance of our work is conferred where, using r s and R, we empirically estimate the oscillation frequency of the shock front (ν QP O ) when it exhibits Quasiperiodic (QP) variations. The obtained results indicate that the present formalism seems to be potentially viable to account for the QPO frequency in the range starting from milli-Hz to kilo-Hz as 0.386 Hz ≤ ν QP O 10M⊙ MBH ≤ 1312 Hz for a k = 0.99, where M BH stands for the black hole mass.

Study of mass outflow rates from magnetized advective accretion disk around rotating black holes

“…In reality, during the course of accretion, rotating matter around black hole experiences centrifugal repulsion that eventually triggers the discontinuous transition of the flow variables in the form of shock waves. Such accretion solutions containing shocks are already studied in both hydrodynamic [32][33][34][35][36][37][38][39][40][41][42] as well as magnetohydrodynamics [21,[43][44][45][46][47][48] frameworks. Due to shock compression, convergent accretion flow becomes hot and dense in the post-shock region (equivalently post-shock corona, hereafter PSC) and therefore, PSC become puffed up resulting an effective boundary layer around the black hole.…”