LANČOVÁ, Debora. GRRMHD simulation of sub-Eddington accretion onto stellar mass black hole. In Texas Symposium on Relativistic Astrophysics. 2022.
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Basic information
Original name GRRMHD simulation of sub-Eddington accretion onto stellar mass black hole
Authors LANČOVÁ, Debora.
Edition Texas Symposium on Relativistic Astrophysics, 2022.
Other information
Original language English
Type of outcome Presentations at conferences
Confidentiality degree is not subject to a state or trade secret
WWW URL
Organization unit Institute of physics in Opava
Changed by Changed by: Mgr. Debora Lančová, Ph.D., učo 33253. Changed: 21/9/2022 09:52.
Abstract
A widely accepted picture of an accretion flow in a soft spectral state X-ray binary system is a geometrically thin disk structure much alike the classic analytic solution of Shakura and Sunyaev. Despite the fact that the analytic models are troubled by instabilities and miss important aspects of physics such as magnetic fields, they are successfully used as a framework for interpreting observational data through continuum spectral fitting. We present results of general relativistic radiative magnetohydrodynamic simulations of sub-Eddington optically thick accretion on a stellar mass black hole with a mildly sub-Eddington luminosity. We find the accretion flow stabilized by magnetic field, with a puffed-up optically thick region, resembling a warm corona surrounding denser disk core. We analyze the inner structure and properties of the puffy disk and compare it with analytical models.
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