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

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.

arXiv commentaccepted by MNRAS

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Cited by in corpus (5)

• The self-similar structure of advection-dominated discs with outflow and radial viscosity
• Viscous accretion of a polytropic self-gravitating disk in the presence of wind
• The influence of winds on the time-dependent behavior of self-gravitating accretion discs
• Numerical study of self-gravitating protoplanetary discs
• Self-gravitational collapse of polytropic mass-losing gaseous discs: effects of outer boundary condition dictated by parent cloud