Other
Scientific paper
Oct 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993rmxaa..26...99a&link_type=abstract
Revista Mexicana de Astronomia y Astrofisica, 26, 99 (1993)
Other
1
Scientific paper
The evolution of the 2.0, 2.2, 2.5., 2.9. 3.5, 4.0, and 6.0 M_sun helium stars was calculated. With the help of a simple method for the determination of the helium convective core-boundary, the influence of overshooting at its edge was accounted. If the helium stars with masses from 6.0 to 2.0 M_sun formed in massive binary systems with separations between the components less than ~2-10 R_sun respectively (the second components are assumed to be compact objects), then they might reach their Roche lobes before the carbon ignition in the core and they will nonconservately lose mass. Such a mass loss phase is numerically investigated. The remnant masses, the duration and other characteristics of this phase are obtained. Helium stars more massive than 2.2 M_sun undergo a SN explosion and form neutron stars (after the mass loss phase). If the system does not disintegrate by the explosion, then it might be the progenitor of a binary radiopulsar. The initial helium-star masses and the orbital separations of such a binary radiopulsar are estimated.
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