The afterclap of degenerate carbon ignition revisited

Details The afterclap of degenerate carbon ignition revisited The afterclap of degenerate carbon ignition revisited

Mar 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980jphys..41c.159b&link_type=abstract

(Centre National de la Recherche Scientifique, Colloque International sur la Physique de la Matiere Dense, Paris, France, Sept.

Physics

Carbon Stars, Convective Heat Transfer, Ignition, Neutron Stars, Stellar Evolution, Thermonuclear Reactions, Combustion Physics, Degeneration

Scientific paper

Whether the degenerate C-O cores, which develop in the heart of 4-8 solar-mass stars, become fully disrupted or implode into neutron stars depends critically on the results of carbon ignition and on the nature of the propagation of the burning front. The velocity of this front is determined by the fastest of several processes, namely (1) detonation, (2) conductive burning, and (3) convective burning. Detonation can probably be excluded because of the small overpressures resulting from burning at high density. Since conductive burning is estimated to be very slow, the burning front is shown to propagate by convection. It is concluded that if ignition occurs at sufficiently high density (exceeding 5 billion g/cu cm), electron captures and concomitant neutrino losses will then offset the effects of burning and cause the implosion of the core.

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