Observational evidence for metallicity-dependence of the Beta Cephei instability strip

Details Observational evidence for metallicity-dependence of the Beta Cephei instability strip Observational evidence for metallicity-dependence of the Beta Cephei instability strip

Nov 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...251...69w&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 251, no. 1, Nov. 1991, p. 69-74.

Astronomy and Astrophysics

Astrophysics

16

B Stars, Metallicity, Stellar Oscillations, Abundance, Stellar Spectrophotometry

Scientific paper

The southern early-B star HD 166540 is shown to be a probable Beta Cephei star with principal pulsation period 0.23299 days. Additional periods are probably present. According to its colors in the Geneva photometric system, the star is significantly hotter than the classical Beta Cephei stars. All recently discovered Beta Cephei stars with galactocentric distances significantly smaller than that of the sun are fairly blue, and the locus of the instability strip can depend on metallicity. The hypothesis is discussed in terms of the recent proposition that the pulsations of Beta Cephei stars are due to an iron-opacity mechanism. The mechanism does not support the sometimes claimed link between Beta Cephei stars and Be stars.

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