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Linear and Nonlinear Pulsations of β Cephei Stars

Published online by Cambridge University Press:  12 April 2016

Arthur N. Cox  and
Stephen W. Hodson
Arthur N. Cox
Affiliation:
Theoretical Division Los Alamos Scientific Laboratory
Stephen W. Hodson
Affiliation:
Theoretical Division Los Alamos Scientific Laboratory

Extract

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The best known β Cephei variable is a α Virginis (Spica) because it is a binary star (P = 4.01 days) and has a interferometer measurement of its angular diameter. In this study to see if the pulsations can be caused by mixing of hydrogen and helium in the semiconvective zone, the parameters we take are 11.5 M⊙, 26,300 K, 6.5 x 1037 erg/s with an envelope composition of Y = 0.28, Z = 0.02. These data agree within the errors of observations as reported recently by Odell (1980), and the theoretical radial fundamental mode period of 0.171 day compares well with the single observed pulsation period of 0.174 day.

Type
III. β-Cephei and 53 Persei Variables
Information
International Astronomical Union Colloquium , Volume 58: Stellar Hydrodynamics , August 1980 , pp. 323 - 327
Copyright
Copyright © Reidel 1980

References

Kato, S. 1966, PASJ 18, p.374.Google Scholar
Odell, A. 1980, Ap. J. 236, p.536.Google Scholar
Shibahashi, and Osaki, Y. 1976, PASJ 28, p.199.Google Scholar
Shobbrook, R. R., Lomb, N. R. and Herbison-Evans, D. 1972, MNRAS 156, p.165.Google Scholar