Evolution of massive close binaries. I - The X-ray binary stage

Details Evolution of massive close binaries. I - The X-ray binary stage Evolution of massive close binaries. I - The X-ray binary stage

Jul 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975ap%26ss..35..241d&link_type=abstract

Astrophysics and Space Science, vol. 35, July 1975, p. 241-247. Fonds de la Recherche Fondamentale Collective

Astronomy and Astrophysics

Astrophysics

34

Binary Stars, Main Sequence Stars, Stellar Evolution, X Ray Sources, Hydrogen, Mass Ratios, Mass Transfer, Stellar Mass Ejection, Supernovae

Scientific paper

X-ray binaries such as Cen X-3, Cyg X-1, Vela X-1, 2U1700- 37, SMC X-1, Cir X-1, with periods ranging from 2~O87 to 12~28, are probably evolution products of massive binary systems. The massive primary starts losing mass after core hydrogen burning and undergoes a supernova explosion. The evolution of binary systems consisting of a 20 M0 primary and secondaries of respec- tively 14, 10, 8 and 6 M0 was computed from Main Sequence stage through the X-ray phase, until the second mass transfer phase. Estimates were performed for the evolution of a secondary of 4 M0. It may be seen that some of these systems during their X-ray phase match the observed mass ratios and periods

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