Structuring the hot advective accretion flow, as a result interaction of plasma with magnetic field

TL;DR

This paper develops a magneto-hydrodynamic model to analyze the self-structuring and evolution of asymmetric, advective accretion disks influenced by magnetic fields, providing detailed insights into their radial structure at key moments.

Contribution

The paper introduces a novel MHD model with 'meeting coefficients' to study the nonlinear feedback and self-structuring of advective accretion disks in magnetic fields.

Findings

Solutions for the radial structure at two key evolutionary moments

Detailed description of disk self-structuring

Insights into nonlinear effects on flow structure

Abstract

We present a magneto-hydrodynamic model developed for investigations of advective non-stationary, asymmetric Keplerian accretion disks in the normal magnetic field. The introduced model allows us to trace the evolution in different fixed moments and to get detailed description of the self-structuring of the disk. We have introduced "meeting coefficients" that define the feedback. It determines the impact from nonlinear effects have over the structure of the flow. We have obtained solutions for the radial structure of the disk for two crucial moments of its evolution.