A new model for white dwarf supernovae

Details A new model for white dwarf supernovae A new model for white dwarf supernovae

Mar 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982natur.296..225c&link_type=abstract

Nature, vol. 296, Mar. 18, 1982, p. 225, 226.

Physics

20

Binary Stars, Neutron Stars, Stellar Models, Supernovae, White Dwarf Stars, Carbon, Oxygen, Stellar Structure

Scientific paper

It is shown here that carbon-oxygen white dwarfs in close binary systems are likely progenitors of neutron stars and Type I supernovae (SN I). This conclusion is supported by different effects associated with crystallization of the carbon-oxygen mixture at relatively low temperatures less than about 5 x 10 to the 7th K and high densities greater than about 5 x 10 to the 9th g/cu cm. In particular, the existence of a pronounced eutectic in the phase diagram of carbon-oxygen mixtures induces carbon-oxygen separation, with oxygen settling at the star's center and carbon being rejected to lower-density layers. This not only favors quiet or nonexplosive collapse, but it may also induce off-center ignitions at variable depths. Their possible correspondence with the fast to slow SN I range is discussed.

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