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 ̃ 2 × 105 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 & 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....
Andrea Miglio, J.M. (2007). Revised instability domains of SPB and β Cephei stars. COMMUNICATIONS IN ASTEROSEISMOLOGY, 151, 48-56 [10.1553/cia151s48].
Revised instability domains of SPB and β Cephei stars
Andrea Miglio;
2007
Abstract
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 ̃ 2 × 105 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 & 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....I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
