Other
Scientific paper
May 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...304..201i&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 304, May 1, 1986, p. 201-216.
Other
31
Binary Stars, Neutron Stars, Stellar Evolution, Stellar Models, White Dwarf Stars, Convective Heat Transfer, Helium, Hertzsprung-Russell Diagram, Roche Limit, Stellar Mass
Scientific paper
The evolution of model close binary components of initial mass 3-7 Msun and of Population I composition is followed from the beginning of the core helium-burning phase. For one set of models, mass loss is initiated at an arbitrary point during the early AGB phase (early case C events) and evolution is followed to the degenerate dwarf stage. For another set of models, mass loss is initiated when hydrogen is reignited and thermal pulses begin (late case C events). It is found that the inclusion of overshoot and semiconvection during the core helium-burning phase has little effect on the relationship between progenitor mass and final degenerate dwarf mass. A new channel for producing both oxygen-neon (ONe) degenerate dwarfs and neutron stars is identified. Involved are stars of initial mass 7. 8.5 Msun which undergo early case C events. For such stars, mass loss from the surface proceeds sufficiently more rapidly than the mass of the hydrogen-exhausted core can be decreased by convective dredge-up that carbon ignition at the center occurs before degeneracy sets in; the remnant of the mass transfer event can evolve into either an ONe degenerate dwarf or a neutron star at a combined frequency that is comparable to the observed rate of supernova formation in the Galaxy. In binary systems in which the primary becomes a neutron star or an ONe degenerate dwarf, the secondary will normally evolve into a CO degenerate dwarf, and common envelope action will lead in some instances to small enough orbital separations that orbital shrinkage due to gravitational wave radiation will again lead to Roche-lobe filling by the CO dwarf. If before the merging and explosion process begins, the heavier compact component is an ONe degenerate dwarf, a supernova-like explosion fueled by the conversion of carbon and oxygen into iron peak nuclei may result, and the light curve and spectrum may be of the Type I "peculiar" variety. The compact remnant remaining after the explosion may be either an ONe degenerate dwarf or a neutron star.
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