White dwarfs and supernovae

Details White dwarfs and supernovae White dwarfs and supernovae

Oct 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981crasb.293..441c&link_type=abstract

Academie des Sciences (Paris), Comptes Rendus, Series II - Mecanique, Physique, Chimie, Sciences de l'Univers, Sciences de la Te

Physics

1

Binary Stars, Carbon Monoxide, Stellar Mass Accretion, Supernovae, White Dwarf Stars, Main Sequence Stars, Neutron Stars, Nuclear Fusion, Roche Limit

Scientific paper

A binary system consisting of a massive CO white dwarf with a mass near the Chandrasekhar limit and a small main sequence star is discussed. It is shown that the convection forces are excluded from the propagation of thermonuclear combustion and the carbon and oxygen are separated during the solidification of the dwarf's core. These two effects, when combined with varying accretion rates, give rise to either total collapse or partial disruption due to off-center ignition of carbon. The accretion is considered in two forms, a minimum rate where matter is accreted from the stellar wind or even from capture from orbit of material caused by gravitational waves, and an elevated rate, due to an overflow of the Roche lobe of the companion star as it extends toward the main sequence star. The CO white dwarfs are proved to be viable parent stars for neutron stars compacted from binary stars with small mass.

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