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Effect of Instability-Generated Clumping on Wind Compressed Disk Inhibition

Published online by Cambridge University Press:  12 April 2016

S. P. Owocki  and
D. H. Cohen
S. P. Owocki
Affiliation:
Bartol Research Institute, University of Delaware, Newark, DE 19350, USA
D. H. Cohen
Affiliation:
Bartol Research Institute, University of Delaware, Newark, DE 19350, USA

Abstract

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In rapidly rotating stars with a purely radially driven stellar wind, conservation of wind angular momentum can lead to formation of an equatorial Wind Compressed Disk (WCD). However, for a line-driven stellar wind, recent 2D hydrodynamical simulations based on a localized, Sobolev treatment of the line-force indicate that nonradial components of the line-force can effectively inhibit formation of such a WCD. This presentation will describe current efforts to extend such 2D simulations to a nonlocal, smooth-source-function treatment of the line-force that can incorporate the intrinsically strong instability of line-driving to formation of small-scale, clumped structure. Key questions are how such small-scale clumped structure affects the nonradial line-force components that arise from large-scale velocity-gradient asymmetries, and in particular whether such nonradial forces can still inhibit WCD formation in a clumped flow. The results have important implications for the viability of the WCD mechanism as a paradigm for disk formation in Be stars.

Type
6. Disks
Information
International Astronomical Union Colloquium , Volume 175: The Be Phenomenon in Early-Type Stars , 2000 , pp. 621 - 625
Copyright
Copyright © Astronomical Society of the Pacific 2000

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