2007CoAst.151...48M

The excitation of pulsation modes in β Cephei and Slowly Pulsating B stars is known to be very sensitive to opacity changes in the stellar interior where T∼2x10⁵K. 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 & 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.