Revised instability domains of SPB and beta Cephei stars

Details Revised instability domains of SPB and beta Cephei stars Revised instability domains of SPB and beta Cephei stars

2007-06-25

arxiv.org/abs/0706.3632v1

Astronomy and Astrophysics

Astrophysics

9 pages, 4 figures. Accepted for publication in Communications in Asteroseismology

Scientific paper

10.1553/cia151s48

The excitation of pulsation modes in beta Cephei and Slowly Pulsating B stars is known to be very sensitive to opacity changes in the stellar interior where T~2 10^5 K. In this region differences in opacity up to ~50% can be induced by the choice between OPAL and OP opacity tables, and between two different metal mixtures (Grevesse and Noels 1993 and Asplund et al. 2005). We have extended the non-adiabatic computations presented in Miglio et al. (2007) towards models of higher mass and pulsation modes of degree l=3, and we present here the instability domains in the HR- and log(P)-log(Teff) diagrams resulting from different choices of opacity tables, and for three different metallicities.

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