Podrobný výpis o publikaci

LANČOVÁ, Debora. GRRMHD simulation of sub-Eddington accretion onto stellar mass black hole. In Texas Symposium on Relativistic Astrophysics. 2022.

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Základní údaje
Originální název	GRRMHD simulation of sub-Eddington accretion onto stellar mass black hole
Autoři	LANČOVÁ, Debora.
Vydání	Texas Symposium on Relativistic Astrophysics, 2022.

Další údaje
Originální jazyk	angličtina
Typ výsledku	Prezentace na konferencích
Utajení	není předmětem státního či obchodního tajemství
WWW	URL
Organizační jednotka	Fyzikální ústav v Opavě
Změnil	Změnila: Mgr. Debora Lančová, Ph.D., učo 33253. Změněno: 21. 9. 2022 09:52.

Anotace
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.

Anotace

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.