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Thermonuclear supernovae: a multi-scale astrophysical problem challenging numerical simulations and visualization
F K Röpke and R Bruckschen 2008 New J. Phys. 10 125009 (20pp)   doi: 10.1088/1367-2630/10/12/125009

Evolution of a merging pair of C+O white dwarfs to form a single neutron star

Abstract. Investigates the evolution of a merging pair of C+O white dwarfs which constitutes a close binary system. The merging process is simulated as a rapid mass transfer from a less massive white dwarf to a more massive one at a rate of 1*10^-5 M_(.) yr^-1. Such a rapid accretion ignites an off-center carbon flash. The authors found that the carbon burning front propagates inward all the way through the central region and hence the CO white dwarf is completely charged into an ONeMg white dwarf in a quiescent manner. Therefore, the ultimate outcome of the system will not be a Type I supernova explosion induced by the carbon deflagration, but a collapse triggered by electron captures on ²⁴Mg and ²⁰Ne to form a single neutron star. This class of neutron star might be an origin of a single millisecond pulsar

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