Neutrino escape, nuclear dissociation, and core collapse and/or explosion

Details Neutrino escape, nuclear dissociation, and core collapse and/or explosion Neutrino escape, nuclear dissociation, and core collapse and/or explosion

Dec 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...263l..55a&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor, vol. 263, Dec. 15, 1982, p. L55-L57. Research supported by the Alexander

Astronomy and Astrophysics

Astrophysics

48

Gravitational Collapse, Neutrinos, Stellar Evolution, Stellar Models, Supernovae, Astronomical Models, Equations Of State, Hydrodynamics, Metallic Stars, Nuclear Astrophysics, Reaction Kinetics

Scientific paper

Extensive numerical calculations of spherically symmetric stellar collapse have been carried out, in which a careful treatment of neutrino transport, equation of state, weak interaction reaction rates, and relativistic hydrodynamics has been attempted. It is shown that, with currently accepted physics of the collapse, the outcome is continued collapse for initial models with large iron cores and a marginal explosion for models with iron cores near 1.4 solar mass. The lack of strong explosions is the result of energy production by the bounce of the inner regions, M(r) = 0.6 solar mass; this energy production is inadequate to dissociate the nuclei remaining in the outer regions of the large cores. Previously neglected effects of pulsational instability during silicon burning in the presupernova star may result in smaller iron cores at collapse and in stronger explosions.

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