THE INSTABILITY STRIP OF β CEPHEI STARS

摘要

A comparison between two different theoretical approaches to the β Cephei instability strip is given in this paper. These works are quite distinct from each other. To find the appropriate one, a statistics based on a sample of 49 stars is presented subsequently. After deriving their effective temperatures and luminosities from their (B - V) , (U - B) colors and parallaxes we find their positions in the HR diagram to be mostly confined to the main sequence. Their masses are between 7 solar mass and 30 solar mass. Comparison with the previous theoretical work shows that the theoretical instability strip, which has an upper bound in the luminosity and rather tight boundaries in the effective temperature, matches observational constraints very well.