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

Abstract

This paper explores the effects of large-scale magnetic fields in hot accretion flows for asymmetric configurations with respect to the equatorial plane. The solutions that we have found show that the large-scale asymmetric magnetic field can significantly affect the dynamics of the flow and also cause notable outflows in the outer parts. Previously, we treated a viscous resistive accreting disc in the presence of an odd symmetric $\text{B-}$ field about the equatorial plane. Now we extend our earlier work by taking into account another configuration of large-scale magnetic field which is no longer symmetric. We provide asymmetric field structures with small deviations from even and odd symmetric $\text{B-}$field. Our results show that the disc's dynamics and appearance become different above and below the equatorial plane. The set of solutions also predicts that even a small deviation in a symmetric field causes the disc to compress on one side and expand on the other. In some cases, our solution represents a very strong outflow from just one side of the disc. Therefore, the solution may potentially explain the origin of one-sided jets in radio galaxies.

accepted for publication in MNRAS

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• Anchoring polar magnetic field in a stationary thick accretion disk
• 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
• Fourier analysis of advection-dominated accretion flows