On Thermal Dis-Equilibrium in Super-Eddington Stars

Details On Thermal Dis-Equilibrium in Super-Eddington Stars On Thermal Dis-Equilibrium in Super-Eddington Stars

Sep 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aspc..332..200g&link_type=abstract

The Fate of the Most Massive Stars, ASP Conference Series, Vol. 332, Proceedings of the conference held 23-28 May, 2004 in Grand

Astronomy and Astrophysics

Astronomy

Scientific paper

The purpose of this contribution is to stimulate general thinking about LBV mass-loss timescales as the expected response to thermal disequilibrium in stars of roughly 100 solar masses. The disequilibrium appears when the star becomes super-Eddington, defined as having a radiative force that exceeds gravity at heights above where the convection is already maximal, i.e., where turnover speeds go transsonic. In this case, the mass-loss timescales may be governed by simple order-unity scaling arguments, which require for self-consistency the appearance of clumpy porosity in the surface layers. The essential ansatz is that the average mass-loss timescale must be of order the thermal adjustment time.

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