Thermal instability of thin disk in the presence of wind and corona

TL;DR

This paper explores how magnetic fields, winds, and coronae influence the thermal stability of thin accretion disks in high-energy astrophysical systems, revealing complex dependencies that affect disk structure and behavior.

Contribution

It provides a comprehensive analysis of the combined effects of magnetic fields, winds, and coronae on disk stability, advancing theoretical understanding and modeling of accretion disks.

Findings

Increasing corona parameters raises disk thickness and reduces temperature.

Magnetic fields can enhance disk stability under certain conditions.

Winds and coronae can either stabilize or destabilize the disk depending on their properties.

Abstract

This study investigates the thermal stability of thin accretion disks in high-energy astrophysical systems, incorporating the effects of magnetic fields, winds, and coronae. We analyze how these factors influence disk stability, focusing on conditions under which magnetic fields enhance stability and on scenarios where winds and coronae can either stabilize or destabilize the disk. Our results reveal that increasing corona parameters raises disk thickness and reduces temperature, thereby affecting gas, radiation, and magnetic pressures. These interactions underscore the complex dependencies that shape accretion disk dynamics, offering insights into their structural and thermal behavior under varying physical conditions. The findings contribute to advancing theoretical models and numerical simulations of accretion processes in environments such as active galactic nuclei (AGN) and X-ray binaries, where disk stability plays a critical role in observed emissions and variability patterns.