The role of thermal conduction in magnetized viscous-resistive ADAFs

TL;DR

This paper investigates how thermal conduction influences the structure of magnetized viscous-resistive advection-dominated accretion flows (ADAFs), highlighting the sensitivity of flow properties to various physical parameters.

Contribution

It presents self-similar solutions for 2D magnetized ADAFs including thermal conduction, a novel aspect in modeling hot accretion flows under weak collision conditions.

Findings

Flow structure depends on viscosity, advection, and thermal conduction.

Radial flow, angular velocity, and density vary with physical parameters.

Thermal conduction significantly impacts the global structure of ADAFs.

Abstract

Observations of the hot gas, which is surrounding Sgr A* and a few other nearby galactic nuclei, imply that mean free paths of electron and proton are comparable to gas capture radius. So, hot accretion flows likely proceed under week collision conditions. As a result thermal conduction by ions has a considerable contribution in transfer of the realized heat in accretion mechanisms. We study a 2D advective accretion disk bathed in a poloidal magnetic field of a central accretor in the presence of thermal conduction. We find self-similar solutions for an axisymmetric, rotating, steady, viscose-resistive, magnetized accretion flow. The dominant mechanism of energy dissipation is assumed to be turbulence viscosity and magnetic diffusivity due to magnetic field of the central accretor. We show that the global structure of ADAFs are sensitive to viscosity, advection and thermal conduction parameters. We discuss how radial flow, angular velocity and density of accretion flows may vary with the advection, thermal conduction and viscous parameters.