Phenomenological photofluiddynamics

Issue		EAS Publications Series Volume 21, 2006 Stellar Fluid Dynamics and Numerical Simulations: From the Sun to Neutron Stars


Page(s)		127 - 145
DOI		10.1051/eas:2006109
Published online		07 June 2006

Stellar Fluid Dynamics and Numerical Simulations: From the Sun to Neutron Stars
M. Rieutord and B. Dubrulle (eds)
EAS Publications Series, 21 (2006) 127-145
DOI: 10.1051/eas:2006109

E.A. Spiegel

Astronomy Deparmtnent, Columbia University, New York, USA

Abstract
Using a variety of laboratory analogues and some simple models, I try to portray the fluid dynamics of very hot stars and disks. By analogy to fluidized beds, we may expect the formation of photon bubbles that stir things up into a sort of turbulence. Because of rotation, the bubbles merge to make vortices whose presence causes inhomogeneous radiative outflows and 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.

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