Stothers and Chin 1973
Stothers, R., and C.-W. Chin, 1973: Evolution of stars with suppressed core convection. Astrophys. J., 180, 901-905.
Stellar evolution on the upper main sequence has been computed for models of stars with cores assumed to be in radiative equilibrium, up to the point of central helium ignition. The role of the Schönberg-Chandrasekhar limit for isothermal core is found to be critical for the evolutionary tracks. Observational data are used to rule out the hypothesis of evolution with radiative cores (in upper main-sequence stars) and, by implication, of magnetic fields that are sufficiently strong to have suppressed the core convection.
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Stothers, R., and Chin, C.-W.: Evolution of stars with suppressed core convection, Astrophys. J., 180, 901-905, 1973.
Stothers, R., and C.-W. Chin (1973), Evolution of stars with suppressed core convection, Astrophys. J., 180, 901-905.
Stothers, R., and C.-W. Chin, 1973: Evolution of stars with suppressed core convection. Astrophys. J., 180, 901-905.
Stothers, R., & Chin, C.-W. 1973, Astrophys. J., 180, 901.
Stothers R, Chin C-W. Evolution of stars with suppressed core convection, Astrophys J 1973;180:901-905.
R. Stothers, C.-W. Chin, Astrophys. J. 180, 901-905 (1973).
