Continuum vs. Line Driven Mass Loss and the Eddington Limit

Details Continuum vs. Line Driven Mass Loss and the Eddington Limit Continuum vs. Line Driven Mass Loss and the Eddington Limit

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...5e...3o&link_type=abstract

Calibrating the Top of the Stellar M-L Relation, 26th meeting of the IAU, Joint Discussion 5, 16 August 2006, Prague, Czech Repu

Physics

Scientific paper

Basic stellar structure dictates that stars of ca. 100 Msun or more will be close to the Eddington limit, with luminosities in excess of 10^6 Lsun, and radiation pressure contributing prominently to the support against gravity. Although it is formally possible to generate static structure models of even more massive stars, there is little or no evidence such stars actually exist. This talk will focus on the role of extreme mass loss is limiting the masses of stars, emphasizing in particular that continuum driving, possibly associated with structural instabilities of radiation dominated envelope, can lead to much stronger mass loss than is possible by the usual line-scattering mechanism of steady stellar winds. I will briefly discuss the implications for the evolution of the most massive stars, including both the first stars and GRB progenitors.

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