How does an asymmetric magnetic field change the vertical structure of a hot accretion flow?

Samadi, Maryam; Abbassi, Shahram; Lovelace, R. V. E.

doi:10.1093/mnras/stx1216

Cited by 15 publications

(6 citation statements)

References 60 publications

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“…Blandford & Begelman 1999;Akizuki & Fukue 2006;Abbassi et al 2008;Zhang & Dai 2008;Bu, Yuan & Xie 2009;Mosallanezhad et al 2012, Abbassi & Mosallanezhad 2012aMosallanezhad et al 2013) and also in two dimensions (e.g. Narayan & Yi 1995a;Xu & Chen 1997;Blandford & Begelman 2004;Xue & Wang 2005;Tanaka & Menou 2006;Jiao & Wu 2011;Mosallanezhad et al 2014;Samadi & Abbassi 2016;Mosallanezhad et al 2016;Samadi et al 2017). It is mentioned here, since the hot accretion flows are geometrically thick, the height-integrated approximation used in one dimensional self-similar solutions is not so appropriate.…”

Section: Introductionmentioning

confidence: 98%

The effects of toroidal magnetic field on the vertical structure of hot accretion flows

Zeraatgari,

Mosallanezhad,

Abbassi

et al. 2017

Preprint

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We solved the set of two-dimensional magnetohydrodynamic (MHD) equations for optically thin black hole accretion flows incorporating toroidal component of magnetic field. Following global and local MHD simulations of black hole accretion disks, the magnetic field inside the disk is decomposed into a large scale field and a fluctuating field. The effects of the fluctuating magnetic field in transferring the angular momentum and dissipating the energy are described through the usual α description. We solved the MHD equations by assuming steady state and radially self-similar approximation in r − θ plane of spherical coordinate system. We found that as the amount of magnetic field at the equatorial plane increases, the heating by the viscosity decreases. In addition, the maximum amount of the heating by the viscous dissipation is produced at the mid-plane of the disk, while that of the heating by the magnetic field dissipation is produced at the surface of the disk. Our main conclusion is that in terms of the no-outflow solution, thermal equilibrium still exists for the strong magnetic filed at the equatorial plane of the disk.

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Section: Introductionmentioning

confidence: 98%

The effects of toroidal magnetic field on the vertical structure of hot accretion flows

Zeraatgari,

Mosallanezhad,

Abbassi

et al. 2017

Preprint

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“…There are several analytical investigations based on the self-similar assumption that probe the magnetic field effects in hot accretion flows (Akizuki & Fukue 2006;Abbassi et al 2008;Zhang & Dai 2008;Bu et al 2009;Mosallanezhad et al 2014;Samadi et al 2017;Bu & Mosallanezhad 2018;Deng & Bu 2019). In practice, the analytical studies are powerful tools to understand the physical properties of inflow and wind from accretion flow.…”

Section: Introductionmentioning

confidence: 99%

Self-similar Solution of Hot Accretion Flow with Thermal Conduction and Anisotropic Pressure

Mosallanezhad,

Zeraatgari,

Mei

et al. 2022

Preprint

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We explore the effects of anisotropic thermal conduction, anisotropic pressure, and magnetic field strength on the hot accretion flows around black holes by solving the axisymmetric, steady-state magnetohydrodynamic equations. The anisotropic pressure is known as a mechanism for transporting angular momentum in weakly collisional plasmas in hot accretion flows with extremely low mass accretion rates. However, anisotropic pressure does not extensively impact the transport of the angular momentum, it leads to shrinkage of the wind region. Our results show that the strength of the magnetic field can help the Poynting energy flux overcomes the kinetic energy flux. This result may be applicable to understand the hot accretion flow in the Galactic Center Sgr A* and M87 galaxy.

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“…While it is much easier to probe the dependency of the results to the input parameters in analytical approach. Based on radial self-similar approximation, the existence of wind have been investigated in more details by solving HD and MHD equations of hot accretion flow (e.g., Bu et al 2009;Jiao & Wu 2011, Mosallanezhad et al 2014Samadi et al 2017;Bu & Mosallanezhad 2018;Kumar & Gu 2018;Zeraatgari et al 2020). Due to the technical difficulties such as the existing of singularity near the rotation axis in these studies the physical boundary conditions set at only the equatorial plane and the equations have been integrated from this boundary.…”

Section: Introductionmentioning

confidence: 99%

Self-similar solution of hot accretion flow: the role of kinematic viscosity coefficient

Zeraatgari,

Mei,

Mosallanezhad

2021

Preprint

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We investigate the dependency of the inflow-wind structure of the hot accretion flow on the kinematic viscosity coefficient. In this regard, we propose a model for the kinematic viscosity coefficient to mimic the behavior of the magnetorotational instability and would be maximal at the rotation axis. Then, we compare our model with two other prescriptions from numerical simulations of the accretion flow. We solve two-dimensional hydrodynamic equations of hot accretion flows in the presence of the thermal conduction. The self-similar approach is also adopted in the radial direction. We calculate the properties of the inflow and the wind such as velocity, density, angular momentum for three models of the kinematic viscosity prescription. On inspection, we find that in the model we suggested wind is less efficient than that in two other models to extract the angular momentum outward where the self-similar solutions are applied. The solutions obtained in this paper might be applicable to the hydrodynamical numerical simulations of the hot accretion flow.

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How does an asymmetric magnetic field change the vertical structure of a hot accretion flow?

Cited by 15 publications

References 60 publications

The effects of toroidal magnetic field on the vertical structure of hot accretion flows

The effects of toroidal magnetic field on the vertical structure of hot accretion flows

Self-similar Solution of Hot Accretion Flow with Thermal Conduction and Anisotropic Pressure

Self-similar solution of hot accretion flow: the role of kinematic viscosity coefficient

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