EAS Publications Series
Volume 21, 2006Stellar Fluid Dynamics and Numerical Simulations: From the Sun to Neutron Stars
|Page(s)||127 - 145|
|Published online||07 June 2006|
M. Rieutord and B. Dubrulle (eds)
EAS Publications Series, 21 (2006) 127-145
Astronomy Deparmtnent, Columbia University,
New York, USA
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.
© EAS, EDP Sciences, 2006
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