General Relativistic Numerical Simulation of sub-Keplerian Transonic Accretion Flows onto Black Holes: Schwarzschild Spacetime

Abstract

We study time evolution of sub-Keplerian transonic accretion flows onto black holes using a general relativistic numerical simulation code. We perform simulations in Schwarzschild spacetime. We first compare one-dimensional simulation results with theoretical results and validate the performance of our code. Next, we present results of axisymmetric, two-dimensional simulation of advective flows. We find that even in this case, for which no complete theoretical analysis is present in the literature, steady state shock formation is possible.

9 pages, 6 figures, Accepted for publication in MNRAS

References in corpus (6)

• Accretion disc viscosity: how big is alpha?
• Periodic massloss from viscous accretion flows around black holes
• The viscosity parameter alpha and the properties of accretion disc outbursts in close binaries
• Effects of Compton Cooling on Outflow in a Two Component Accretion Flow around a Black Hole: Results of a Coupled Monte Carlo-TVD Simulation
• Quasi-Spherical, Time-Dependent Viscous Accretion Flow: One-Dimensional Results
• Segregation of a Keplerian disc and sub-Keplerian halo from a Transonic flow around a Black Hole by Viscosity and Cooling processes

Cited by in corpus (3)

• Low angular momentum relativistic hot accretion flow around Kerr black holes with variable adiabatic index
• Accretion-ejection in rotating black holes: a model for `outliers' track of radio-X-ray correlation in X-ray binaries
• Spectral and Temporal Studies of Swift\,J1658.2--4242 using {\it AstroSat} Observations with {\tt JeTCAF} Model