Unveiling the internal structure of massive supergiants: HD 163899

Details Unveiling the internal structure of massive supergiants: HD 163899 Unveiling the internal structure of massive supergiants: HD 163899

Jul 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009coast.158..308g&link_type=abstract

"Communications in Asteroseismology, Vol.158, p. 308 Proceedings of "38th Liege International Astrophysical Colloquium: Evoluti

Astronomy and Astrophysics

Astrophysics

3

Scientific paper

Supergiant massive stars are post-main sequence stars. During the H shell burning phase of evolution, they present a radiative core in which a strong damping prevents the pulsation modes from being excited. However Saio et al. (2006) have recently highlighted p and g pulsation modes in a post-main sequence star (HD 163899) observed by MOST. They suggest that the presence of an intermediate convective region (ICZ) at the top of the radiative core allows a partial or total reflexion of the mode. Through some numerical results achieved with CLES (Scuflaire et al. 2008) and MAD (Dupret et al. 2003) codes, we show that this scenario depends on the evolution stage of the star and on the considered mass loss rate and overshooting parameter.

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