Astronomy and Astrophysics – Astrophysics
Scientific paper
Aug 1976
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976ap%26ss..43...35d&link_type=abstract
Astrophysics and Space Science, vol. 43, Aug. 1976, p. 35-46. Fonds National de la Recherche Scientifique
Astronomy and Astrophysics
Astrophysics
17
Binary Stars, Stellar Evolution, Stellar Mass, White Dwarf Stars, Carbon, Computerized Simulation, Helium, Mass Transfer, Neutrinos, Nuclear Fusion
Scientific paper
The evolution of a binary system with components of 10 and 8 solar masses is computed through case B of mass exchange. It is found that after the end of core helium burning, a second stage of mass transfer from the primary occurs. Carbon ignition is prohibited by the large neutrino losses in the degenerate core. The primary remnant, a 1.12-solar-mass star, ends as a white dwarf. A comparison with the 10-solar-mass single evolution is made.
de Greve Jean-Pierre
de Loore Camiel
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