Publication Abstracts

Stothers 1965

Stothers, R., 1965: On the evolutionary state of β Cephei stars. Astrophys. J., 141, 671-687, doi:10.1086/148154.

An attempt is made to explain the β Cephei variables as non-rotating stars undergoing radial oscillations, on the basis of their relatively low observed rotational velocities and the period analyses by van Hoof. Arguments based on the central condensation and on the time scale of evolution vis-a-vis their observed numbers indicate that these BO.5-B2 giants are in the hydrogen-burningphase. Model sequences are constructed for stars of 15 and 20 M to the end of hydrogen burning. The pulsational characteristics are then obtained by perturbing the stable models in the usual adiabatic approximation. The results show that, at some central hydrogen abundance which is higher for the lower masses, the periods and their ratios may be accounted for. Ideally, these quantities imply a unique mass and mean molecular weight for each observed star on the H-R diagram, but comparison of theory and observation gives at present merely a mass range of 10-20 and probably a "normal" chemical composition. At any rate, the hypothesis of evolution of main-sequence O9-B1 stars across the instability strip seems to be correct. Uncertainties in the semiconvective theory of massive stars would appear to be irrelevant since the quasi-stable zone has almost no effect on the pulsational eigenfrequencies. Several lines of observational evidence tend to confirm the theoretical results that β Cephei stars of lower mass fall closer to the initial main sequence. The Wolf-Rayet objects form an apparent extension of the instability strip to higher masses (O stars).

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BibTeX Citation

  author={Stothers, R.},
  title={On the evolutionary state of β Cephei stars},
  journal={Astrophys. J.},

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RIS Citation

ID  - st07710h
AU  - Stothers, R.
PY  - 1965
TI  - On the evolutionary state of β Cephei stars
JA  - Astrophys. J.
VL  - 141
SP  - 671
EP  - 687
DO  - 10.1086/148154
ER  -

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