Publication Abstracts

Stothers and Chin 1968

Stothers, R., and C.-W. Chin, 1968: Evolution of massive helium-burning supergiants. Astrophys. J., 152, 225-232, doi:10.1086/149540.

Models have been constructed for massive stars of 15, 60, and 100 M in the core helium-burning phase of evolution Their luminosity remains nearly constant during evolution and is relatively insensitive to uncertainties in the interior structure, whereas the effective temperature is definitely not. Previously published models in which the opacity was taken to be only electron scattering or in which the envelope instability was treated as fully convective start helium burning as blue supergiants With the inclusion of bound-free absorption and semiconvective mixing, the models start as red supergiants, then move to the blue region The effective temperature of blue supergiants may also be lowered by increasing the hydrogen, metals, and/or CNO abundances. The fraction of time spent in the blue region and the maximum effective temperature attained are probably both larger at higher masses. However, these are very sensitive to conditions in the previous red-supergiant phase. Subsequent to the blue phase, the stars are expected to burn carbon (in a second red-supergiant phase) We suggest that the red supergiants in young clusters like h and χ Per may be, at least in part, in the core helium-burning phase of evolution.

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BibTeX Citation

  author={Stothers, R. and Chin, C.-W.},
  title={Evolution of massive helium-burning supergiants},
  journal={Astrophys. J.},

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RIS Citation

ID  - st06910w
AU  - Stothers, R.
AU  - Chin, C.-W.
PY  - 1968
TI  - Evolution of massive helium-burning supergiants
JA  - Astrophys. J.
VL  - 152
SP  - 225
EP  - 232
DO  - 10.1086/149540
ER  -

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