Abstract
Since the collisional mean free path of charged particles in hot accretion flows can be significantly larger than the typical length-scale of the accretion flows, the gas pressure is anisotropic to magnetic field lines. For such a large collisional mean free path, the resistive dissipation can also play a key role in hot accretion flows. In this paper, we study the dynamics of resistive hot accretion flows in the presence of anisotropic pressure. We present a set of self-similar solutions where the flow variables are assumed to be a function only of radius. Our results show that the radial and rotational velocities and the sound speed increase considerably with the strength of anisotropic pressure. The increase in infall velocity and in sound speed are more significant if the resistive dissipation is taken into account. We find that such changes depend on the field strength. Our results indicate that the resistive heating is $10\%$ of the heating by the work done by anisotropic pressure when the strength of anisotropic pressure is 0.1. This value becomes higher when the strength of anisotropic pressure reduces. The increase in disk temperature can lead to heating and acceleration of the electrons in such flows. It helps us to explain the origin of phenomena such as the flares in Galactic Center Sgr A*.
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