Sequences of model stars of decreasing mass in thermal equilibrium

Details Sequences of model stars of decreasing mass in thermal equilibrium Sequences of model stars of decreasing mass in thermal equilibrium

Feb 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977sva....21...61k&link_type=abstract

(Astronomicheskii Zhurnal, vol. 54, no. 1, 1977, p. 107-114.) Soviet Astronomy, vol. 21, Jan.-Feb. 1977, p. 61-65. Translation.

Astronomy and Astrophysics

Astronomy

1

Binary Stars, Chemical Composition, Stellar Evolution, Stellar Mass Ejection, Stellar Models, Helium, Hydrogen, Stellar Envelopes, X Ray Sources

Scientific paper

Nonevolutionary sequences of LTE stellar models with decreasing hydrogen-shell masses are calculated which represent stars at the stage of core helium burning. Initial masses of 16, 18, 20, 24, 32, and 64 solar masses are selected, and it is assumed that the Schwarzschild criterion for convective stability is satisfied. The results are used to analyze the mass-loss behavior of close-binary components filling their Roche lobes. It is shown that such primaries in binary systems with an initial primary mass not exceeding about 19 solar masses and a primary/secondary mass ratio of the order of unity should lose mass on a thermal time scale, while primaries exceeding this limit should lose mass on the time scale of core helium burning. The corresponding limit is found to be about 24 solar masses for a primary/secondary mass ratio of the order of 3.

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