Abstract
We show 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 (T ≲ 5×107 K) and high densities (ρ ≳ 5×109g cm−3). 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 centre and carbon being rejected to lower-density layers. This not only favours ‘quiet’ or non-explosive collapse, but it may also induce off-centre ignitions at variable depths. We discuss their possible correspondence with the ‘fast’ to ‘slow’ SN I range.
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Canal, R., Isern, J. & Labay, J. A new model for white dwarf supernovae. Nature 296, 225–226 (1982). https://doi.org/10.1038/296225a0
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DOI: https://doi.org/10.1038/296225a0
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