Solid white dwarfs, neutron stars, and type I supernovae

Details Solid white dwarfs, neutron stars, and type I supernovae Solid white dwarfs, neutron stars, and type I supernovae

Jan 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...117l...1l&link_type=abstract

Astronomy and Astrophysics, vol. 117, no. 1, Jan. 1983, p. L1-L4.

Astronomy and Astrophysics

Astrophysics

8

Neutron Stars, Stellar Mass Accretion, Stellar Models, Supernovae, White Dwarf Stars, X Ray Sources, Binary Stars, Galactic Bulge, Gravitational Collapse, Stellar Evolution, Stellar Temperature

Scientific paper

Consideration is given to models of mass accretion onto initially cold (temperature less than 5 x 10 to the 7th K), massive (mass greater than about 1.2 solar masses) carbon-oxygen white dwarfs as a possible explanation for the range of characteristics of type I supernovae and the presence of neutron stars in low-mass binary systems. Quasi-static calculations are performed for models of such white dwarfs, which, in contrast to previously studied situations, have solid cores, as a function of accretion rate for conditions of complete mixing, the complete separation of an oxygen core and a carbon mantle, and a solid oxygen core surrounded by a fluid carbon-oxygen mantle. It is shown that the relative slowness of burning propagation when conduction is the sole mechanism and eutective phase separation would favor at least a partial stellar collapse, which could explain the galactic bulge X-ray sources. On the other hand, the models with partial chemical separation may provide a range of off-center explosions which might explain nonuniformities in SN I characteristics.

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