Modeling pulsations in hot stars with winds

Details Modeling pulsations in hot stars with winds Modeling pulsations in hot stars with winds

Oct 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008jphcs.118a2019n&link_type=abstract

Journal of Physics: Conference Series, Volume 118, Issue 1, pp. 012019 (2008).

Physics

Scientific paper

The interaction pulsation/mass loss takes different aspects. Pulsations can trigger mass loss as in LBVs and Miras; on the other hand, mass loss can modify the driving conditions within the stars. But the most spectacular aspect is the effect on stellar models which, in turn, opens a royal way to asteroseismology to test physical conditions inside massive stars, such as the extent of convective cores or the appearance of new driving mechanisms. We start with a discussion on MS stars and their strange mode instabilities. We then move on to the excitation of the LBV phenomenon. WR stars and the newly observed MOST period in WR123 are discussed in view of the power of asteroseismology. We then turn to B supergiants, in particular HD163899, and show how asteroseismology can really probe convection, semiconvection and mass loss.

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