MOSALLANEZHAD, Amin, De-Fu BU, Miljenko ČEMELJIĆ, Fatemeh Zahra ZERAATGARI, Yang HAI and Liquan MEI. Numerical Simulation of Hot Accretion Flow around Bondi Radius. Astrophysical Journal. GB - Spojené království Velké Británie a, 2022, vol. 939, No 1, p. "12-1"-"12-12", 12 pp. ISSN 0004-637X. Available from: https://dx.doi.org/10.3847/1538-4357/ac9379.
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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
Original language English
Type of outcome Article in a journal
Field of Study 10308 Astronomy
Country of publisher United Kingdom of Great Britain and Northern Ireland
Confidentiality degree is not subject to a state or trade secret
WWW 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 FÚ, RIV23
Tags International impact, Reviewed
Changed by Changed by: Mgr. Pavlína Jalůvková, učo 25213. Changed: 6/3/2023 08:32.
Abstract
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.
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