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Phenomenological photofluiddynamics

Published online by Cambridge University Press:  07 June 2006

M. Rieutord ,
B. Dubrulle  and
E.A. Spiegel
E.A. Spiegel*
Affiliation:
Astronomy Deparmtnent, Columbia University, New York, USA
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Abstract

Using a variety of laboratory analogues and some simple models, Itry to portray the fluid dynamics of very hot stars and disks. By analogy to fluidizedbeds, we may expect the formation of photon bubbles that stir things up intoa sort of turbulence. Because of rotation, the bubbles merge tomake vortices whose presence causes inhomogeneous radiative outflowsand produces spots. These phenomena will allow the Eddington limit to be exceeded and, where the radiative outflows are locally large, mass loss will be encouraged.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 21: Stellar Fluid Dynamics and Numerical Simulations: From the Sun to Neutron Stars , 2006 , pp. 127 - 145
Copyright
© EAS, EDP Sciences, 2006

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