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Paper IPM / Astronomy / 12906  


Abstract:  
We have studied the structure of hot accretion flow bathed in a general largescale magnetic field. We have considered magnetic parameters β_{r,φ,z}[=c^{2}_{r,φ,z}/(2c^{2}_{s})] , where c^{2}_{r, 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 = αc_{s} H) , with both c_{s} and H as a function of magnetic field. As a result in our model, the kinematic viscosity and magnetic diffusivity (η = η_{0}c_{s} H) are not constant. In order to solve the integrated equations that govern the behavior of the accretion flow, a selfsimilar 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 SubKeplerian for all values of magnetic field parameters, but the rotational velocity can be SuperKeplerian 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.
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