Revised instability domains of SPB and β Cephei stars

@article{Miglio2007RevisedID,
  title={Revised instability domains of SPB and $\beta$ Cephei stars},
  author={Andrea Miglio and Josefina Montalb{\'a}n and M. Li{\`e}ge and Observatoire de Paris and Lesia},
  journal={Communications in Asteroseismology},
  year={2007},
  volume={151},
  pages={48-56}
}
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 × 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 & 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… 

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References

SHOWING 1-5 OF 5 REFERENCES
Revised instability domains of SPB and β Cephei
  • Physics Letters B 591,
  • 2005
La formation desdeséléments chimiques
  • La formation desdeséléments chimiques
  • 1993
Ap&SS, in press
  • ApJ 576,
  • 2002
CoAst, in press
  • Memorie della Societa Astronomica Italiana,
  • 2006
Physics Letters B
  • Physics Letters B
  • 2004