“School of Astronomy”Back to Papers Home
Back to Papers of School of Astronomy
|Paper IPM / Astronomy / 12906||
We have studied the structure of hot accretion flow bathed in a general large-scale magnetic field. We have considered magnetic parameters βr,φ,z[=c2r,φ,z/(2c2s)] , where c2r, φ, z are the Alfvén sound speeds in three direction of cylindrical coordinate (r,φ,z) . The dominant mechanism of energy dissipation is assumed to be the magnetic diffusivity due to turbulence and viscosity in the accretion flow. Also, we adopt a more realistic model for kinematic viscosity (ν = αcs H) , with both cs and H as a function of magnetic field. As a result in our model, the kinematic viscosity and magnetic diffusivity (η = η0cs H) are not constant. In order to solve the integrated equations that govern the behavior of the accretion flow, a self-similar method is used. It is found that the existence of magnetic resistivity will increase the radial infall velocity as well as sound speed and vertical thickness of the disk. However the rotational velocity of the disk decreases by the increase of magnetic resistivity. Moreover, we study the effect of three components of global magnetic field on the structure of the disk. We found out that the radial velocity and sound speed are Sub-Keplerian for all values of magnetic field parameters, but the rotational velocity can be Super-Keplerian by the increase of toroidal magnetic field. Also, Our numerical results show that all components of magnetic field can be important and have a considerable effect on velocities and vertical thickness of the disk.
Download TeX format
|back to top|