Abstract
The long-term evolution of accreting C-O white dwarfs as a possible source of neutron stars and/or SNI events is considered. The effects of solidification of the star’s core are included, in particular carbon-oxygen separation. Different degrees of chemical differentiation and a wide range of accretion rates are studied. We determine the pre-flash configurations and we show that a variety of results are possible, ranging from total collapse to partial disruption due to off-centre ignition of carbon.
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© 1982 D. Reidel Publishing Company
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Canal, R., Isern, J., Labay, J. (1982). Carbon-Oxygen White Dwarf Presupernova Models. In: Rees, M.J., Stoneham, R.J. (eds) Supernovae: A Survey of Current Research. NATO Advanced Study Institutes Series, vol 90. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-7876-8_11
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DOI: https://doi.org/10.1007/978-94-009-7876-8_11
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