Effect of magnetic flux advection on the dynamics of shock in accretion flow around a rotating black hole  

作　　者：Biplob Sarkar Anjali Rao 

机构地区：[1]Faculty of Science&Technology,The ICFAI University Tripura,Agartala,799210,India [2]Department of Physics and Astronomy,University of Southampton.Highfield.Southampton SO 171BJ,UK [3]Department of Applied Sciences,Tezpur University,Napaam-784028.Tezpur,Assam,India

出　　处：《Research in Astronomy and Astrophysics》2020年第3期150-161,共12页天文和天体物理学研究（英文版）

基　　金：a Commonwealth Rutherford Fellowship.

摘　　要：We investigate the dynamical behavior of a magnetized,dissipative accretion flow around a rapidly rotating black hole.We solve the magnetohydrodynamic equations and calculate the transonic accretion solutions which may contain discontinuous shock transitions.We investigate the effect ofζ-parameter(parametrizing the radial variation of the toroidal magnetic flux advection rate)on the dynamical behavior of shocks.For a rapidly rotating black hole and for fixed injection parameters at the outer edge,we show that stationary shocks are sustained in the global magnetized accretion solutions for a wide range ofζand accretion rate(˙m).To investigate the observational implications,we consider dissipative shocks and estimate the maximum accessible energy from the post-shock corona(PSC)for nine stellar mass black hole candidates.We compare this with the observed radio jet kinetic power reported in the literature,whenever available.We find close agreement between the estimated values from our model and those reported in the literature.We investigate the dynamical behavior of a magnetized, dissipative accretion flow around a rapidly rotating black hole. We solve the magnetohydrodynamic equations and calculate the transonic accretion solutions which may contain discontinuous shock transitions. We investigate the effect of ζ-parameter(parametrizing the radial variation of the toroidal magnetic flux advection rate) on the dynamical behavior of shocks. For a rapidly rotating black hole and for fixed injection parameters at the outer edge, we show that stationary shocks are sustained in the global magnetized accretion solutions for a wide range of ζ and accretion rate( ˙m). To investigate the observational implications, we consider dissipative shocks and estimate the maximum accessible energy from the post-shock corona(PSC) for nine stellar mass black hole candidates. We compare this with the observed radio jet kinetic power reported in the literature, whenever available. We find close agreement between the estimated values from our model and those reported in the literature.

关 键 词：accretion accretion discs-magnetohydrodynamics-stars black holes-shock waves-ISM jets and OUTFLOWS 

分 类 号：P145.8[天文地球—天体物理]