Origin and evolution of close binary stars with helium donors

Details Origin and evolution of close binary stars with helium donors Origin and evolution of close binary stars with helium donors

Dec 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989azh....66.1172t&link_type=abstract

Astronomicheskii Zhurnal (ISSN 0004-6299), vol. 66, Nov.-Dec. 1989, p. 1172-1188. In Russian.

Astronomy and Astrophysics

Astronomy

16

Binary Stars, Dwarf Stars, Helium, Neutron Stars, Stellar Evolution, Black Holes (Astronomy), Hertzsprung-Russell Diagram, Milky Way Galaxy, Roche Limit, Stellar Mass Accretion, Supernovae

Scientific paper

This paper is devoted to a numerical study of the origin and evolution of close binary systems consisting of a neutron star or carbon-oxygen dwarf primary and a nondegenerate helium secondary that fills its Roche lobe under the action of gravitational radiation. The rate of formation of such systems in the Galaxy is about 0.017 per year. Analysis of the behavior of the accreted degenerate helium companion reveals two basic possibilities for the evolution of such systems: merging of the components into a single star with a helium envelope, or recurrent dwarf supernova explosions which may resemble the 1885 supernova in N 31. These binaries may also exist for a long time as low mass X-ray binaries, if the primary is a neutron star or a black hole.

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