Physics
Scientific paper
Sep 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987pazh...13..780t&link_type=abstract
Pis'ma v Astronomicheskii Zhurnal (ISSN 0320-0108), vol. 13, Sept. 1987, p. 780-788. In Russian. In Russian. In Russian.
Physics
5
Dwarf Stars, Stellar Evolution, Stellar Physics, X Ray Binaries, Degenerate Matter, Mass Flow Rate, Neutron Stars, Stellar Mass Accretion, Stellar Winds
Scientific paper
The evolutionary status of secondaries in X-ray binaries with orbital periods P < 1h is discussed. Most probably they are degenerate hydrogen-helium dwarfs, which are remnants of stars, that had filled their Roche lobes in the core hydrogen exhaustion stage. However, they may be as well nondegenerate helium stars or helium or carbon-oxygen degenerate dwarfs. The absence of bright X-ray sources with P = 2h - 4h can be explained by an interruption of mass exchange, caused by the switch-off of the magnetic stellar wind. At P < 2h accretion onto a rapidly spinning weakly magnetized neutron star is impossible due to "propeller" action. Only systems that evolve to ultra-short periods could become bright X-ray sources, because they have high enough values of Mat P ⪉ 1h.
Ergma E. V.
Fedorova Alexandra V.
Tutukov Aleksandr V.
Yungelson Lev R.
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