Phenomenological Photofluiddynamics
نویسنده
چکیده
Ledoux cited his estimate of the critical mass (1941) and the later one of Härm and Schwarzschild (1959) in the 50-60 M! range, with the possibility of perhaps 80 M! for metal poor stars. Of course, one may argue that the vibrations may not destroy the star, so de Jager’s question had a point. On the other hand there was also Eddington’s earlier work (1921) in which he derived the stellar luminosity above which the outward force of emerging radiation on the outer layers exceeds the surface gravity. We shall formulate this Eddington limit below. Together with the mass-luminosity relation, the Eddington limit had for years been considered to impose an upper bound on possible stellar masses. However, there are observations indicating that stars do exist above this limit and so it is worth examining the fluid dynamical issues that arise in the envelopes of massive stars. Perhaps that is what de Jager had in mind in raising this issue. The fluid dynamical processes that I shall discuss qualitatively here — photon bubbles and vortices — are what may allow a star to exist above the Eddington limit but, even with these, a very luminous star probably cannot keep all its mass indefinitely. So the question has to be rephrased
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