Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...178..170v&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 178, no. 1-2, May 1987, p. 170-178. ZWO-supported research.
Astronomy and Astrophysics
Astrophysics
24
B Stars, Binary Stars, Mass Transfer, Stellar Evolution, Stellar Models, Computerized Simulation, Helium, Isotopes, Nuclear Fusion, Stellar Cores
Scientific paper
Numerical simulations of close binary evolution were carried out for five binary systems with masses 3+2, 4+3.2, 6+4, 9+6, 12+8 M_sun; and periods 2d, 1d.78, 3d, 4d, 5d respectively. The primary component of these systems was followed from the zero-age main sequence through the mass transfer phase and into core-helium burning. The five systems appear to follow an almost homologous evolution, presumably as a consequence of the particular choice of the initial mass ratios and binary periods. After the mass transfer phase the resulting systems consist of a main-sequence star with a helium star companion of mass 0.36, 0.46, 0.82, 1.48, 2.30 M_sun; for the five systems, respectively. The properties of the resulting systems are compared with the characteristics of B-emission stars. It is shown that the statistical properties of Be stars can be interpreted in terms of a binary model.
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