The influence of winds on the time-dependent behavior of self-gravitating accretion discs

TL;DR

This paper investigates how winds affect the evolution of self-gravitating, isothermal accretion discs, revealing that winds reduce surface density and alter radial velocities, especially in the outer regions, with minimal impact on the inner core.

Contribution

It provides a semi-analytical, similarity solution for the time evolution of self-gravitating accretion discs considering radius-dependent wind effects, highlighting structural differences.

Findings

Winds decrease surface density in inner and outer disc regions.

Radial velocity increases significantly in the outer disc due to winds.

The inner disc region shrinks with stronger winds.

Abstract

We study effects of winds on the time evolution of isothermal, self-gravitating accretion discs by adopting a radius dependent mass loss rate because of the existence of the wind. Our similarity and semi-analytical solution describes time evolution of the system in the slow accretion limit. The disc structure is distinct in the inner and outer parts, irrespective of the existence of the wind. We show that existence of wind will lead to a reduction of the surface density in the inner and outer parts of the disc in comparison to a no-wind solution. Also, the radial velocity significantly increases in the outer part of the disc, however, the accretion rate decreases due to the reduced surface density in comparison to the no-wind solution. In the inner part of the disc, mass loss due to the wind is negligible according to our solution. But the radial size of this no-wind inner region becomes smaller for stronger winds.