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2010MNRAS.401..177C - Mon. Not. R. Astron. Soc., 401, 177-190 (2010/January-1)
Mass loss from the inner regions of accretion discs due to centrifugally driven magnetic wind flows.
CAMPBELL C.G.
Abstract (from CDS):
It is shown here that if the standard boundary condition of vanishing viscous stress close to the stellar surface is applied, together with the standard connection between viscosity and magnetic diffusivity, then poloidal magnetic field bending increases as the star is approached with a corresponding increase in the wind mass loss rate. A significant amount of material can be lost from the system via the enhanced wind from a narrow region close to the stellar surface. This occurs for a Keplerian angular velocity distribution and for a modified form of angular velocity, which allows for matching of the disc and stellar rotation rates through a boundary layer above the stellar surface. The enhanced mass loss is significantly affected by the behaviour of the disc angular velocity as the stellar surface is approached, and hence by the stellar rotation rate. Such a mechanism may be related to the production of jets from the inner regions of disc accreting systems.
Abstract Copyright: © 2009 The Authors. Journal compilation © 2009 RAS
Journal keyword(s): accretion, accretion discs - magnetic fields - MHD - ISM: jets and outflows
Simbad objects: 2
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