General Relativistic Numerical Simulation of sub-Keplerian Transonic Accretion Flows onto Rotating Black Holes: Kerr 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 around the black holes having non-zero rotation. 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. In the literature, there is no solution which describes steady shock solutions in two dimensions. However, our simulations produce these centrifugal force supported steady shock waves even in presence of strong dragging of inertial frames. Since the post-shock region could be hot and upscatter photons through Comptonization, these shock would put imprints on the spectra. Thus, our solutions, which represent truly new results, could be useful to measure spins through radiation spectrum of accreting Kerr black holes.

arXiv commentAccepted for publication in MNRAS

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Cited by in corpus (8)

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• Low angular momentum relativistic hot accretion flow around Kerr black holes with variable adiabatic index
• General relativistic hydrodynamic simulations of perturbed transonic accretion
• Three Dimensional Simulations of Advective, Sub-Keplerian Accretion Flow onto Non-rotating Black Holes
• Evidence of Outflow Induced Soft Lags of Galactic Black Holes
• Effects of resistivity on standing shocks in low angular momentum flows around black holes
• Detection of QPO Soft Lag during Outburst of Swift J1727.8-1613: Estimation of Instrinsic Parameters from Spectral Study
• General relativistic viscous accretion flow around Konoplya-Zhidenko black hole