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Selfconsistent Models of Winds from Rotating Early-Type Stars – Application to B[e] star winds
Published online by Cambridge University Press: 12 April 2016
Abstract
We present results of 2.5-D radiation hydrodynamical simulations of winds from rapidly rotating stars. For the first time, we consider the dependence of the line statistics on local density and radiation temperature implying a spatial variation of the force-multiplier parameters k, α and δ which control the dynamics of the flow.
We apply our models to the problem of disk formation in B[e]-star winds.
- Type
- 6. Disks
- Information
- International Astronomical Union Colloquium , Volume 175: The Be Phenomenon in Early-Type Stars , 2000 , pp. 626 - 631
- Copyright
- Copyright © Astronomical Society of the Pacific 2000