Hydrodynamical wind on a magnetized ADAF with thermal conduction

TL;DR

This paper models how hydrodynamical winds affect the structure and thermal properties of magnetized advection-dominated accretion flows, highlighting the importance of winds in energy and temperature regulation.

Contribution

It introduces self-similar solutions for magnetized ADAFs with thermal conduction considering hydrodynamical winds, revealing their impact on accretion velocity, temperature, and rotational limits.

Findings

Winds decrease disk temperature and luminosity.

Higher wind strength allows larger magnetic field parameters.

Accretion rate decreases with radius in the presence of winds.

Abstract

We examine the effects of a hydrodynamical wind on advection dominated accretion flows with thermal conduction in the presence of a toroidal magnetic field under a self-similar treatment. The disk gas is assumed to be isothermal. For a steady state structure of such accretion flows a set of self similar solutions are presented. The mass-accretion rate $\dot{M}$ decreases with radius $r$ as $\dot{M}\propto r^{s+1/2}$, where $s$ is an arbitrary constant. We show that existence of wind will lead to enhance the accretion velocity. Cooling effects of outflows or winds are noticeable and should be taken into account for calculating luminosity and effective temperature of optically thin and thick ADAFs. Increasing the effect of wind, decreases the disk's temperature, because of energy flux which is taken away by winds. We will see that for a given set of input parameters, the solution reaches to a non-rotating limit at a specific value of $\phi_s$. The values of this limitation on $\phi_s$ will increase by adding $s$, wind parameter. In fact, the higher values of $s$ will allow the disk to have physical rotating solution for larger $\phi_s$.