J 2022

Numerical Simulation of Hot Accretion Flow around Bondi Radius

MOSALLANEZHAD, Amin, De-Fu BU, Miljenko ČEMELJIĆ, Fatemeh Zahra ZERAATGARI, Yang HAI et. al.

Basic information

Original name

Numerical Simulation of Hot Accretion Flow around Bondi Radius

Authors

MOSALLANEZHAD, Amin (191 Croatia), De-Fu BU, Miljenko ČEMELJIĆ (191 Croatia, belonging to the institution), Fatemeh Zahra ZERAATGARI, Yang HAI and Liquan MEI

Edition

Astrophysical Journal, GB - Spojené království Velké Británie a, 2022, 0004-637X

Other information

Language

English

Type of outcome

Článek v odborném periodiku

Field of Study

10308 Astronomy

Country of publisher

United Kingdom of Great Britain and Northern Ireland

Confidentiality degree

není předmětem státního či obchodního tajemství

References:

URL

RIV identification code

RIV/47813059:19630/22:A0000225

Organization unit

Institute of physics in Opava

DOI

http://dx.doi.org/10.3847/1538-4357/ac9379

UT WoS

000874223300001

Keywords in English

advection-dominated accreation;angular momentum material;black holes;thermal conduction;disks;gas;instability;density;models;origin

Tags

, RIV23

Tags

International impact, Reviewed
Změněno: 6/3/2023 08:32, Mgr. Pavlína Jalůvková

Abstract

V originále

Previous numerical simulations have shown that strong winds can be produced in the hot accretion flows around black holes. Most of those studies focus only on the region close to the central black hole; therefore it is unclear whether the wind production stops at large radii around Bondi radius. Bu et al. (2016) studied the hot accretion flow around the Bondi radius in the presence of nuclear star gravity. They find that, when the nuclear stars gravity is important-comparable to the black hole gravity, winds cannot be produced around the Bondi radius. However, for some galaxies, the nuclear stars gravity around Bondi radius may not be strong. In this case, whether winds can be produced around Bondi radius is not clear. We study the hot accretion flow around Bondi radius with and without thermal conduction by performing hydrodynamical simulations. We use the virtual particles trajectory method to study whether winds exist based on the simulation data. Our numerical results show that, in the absence of nuclear stars gravity, winds can be produced around Bondi radius, which causes the mass inflow rate to decrease inwards. We confirm the results of Yuan et al. (2012), which indicate this is due to the mass loss of gas via wind rather than convectional motions.
Displayed: 24/12/2024 03:32