Statistics – Computation
Scientific paper
Jul 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...412..192b&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 412, no. 1, p. 192-202.
Statistics
Computation
40
Computational Astrophysics, Neutrinos, Nuclear Astrophysics, Stellar Interiors, Supernova 1987A, Electron Capture, Shock Fronts, Shock Waves, Stellar Convection, Stellar Mass Accretion, Stellar Structure, Temperature Distribution
Scientific paper
Starting from Wilson's (1982) idea that the supernova gets its energy from neutrinos heating the mantle of the star, I use the neutrino observations to find the available neutrino flux. This agrees well with computations by Wilson and Mayle (1989), using 'neutron fingers'. In the mantle of the star, one can define a 'gain radius': outside this radius, the energy gain from neutrino absorption is greater than the energy loss by electron capture. The temperature and density are calculated from simple arguments for r greater than 100 km. In the region where free nucleons dominate, the entropy is assumed to be constant; in the region where nucleons and alpha particles are mixed, the fraction of nucleons is determined from the internal energy. One can then calculate the fraction of neutrino energy which can be transferred to the region outside the gain radius; this turns out to be 1-2 percent. With the observed neutrino flux, this gives a supernova energy of 0.8 foe (1 foe = 10 exp 51 ergs); nucleosynthesis adds about 0.4 foe, for a total of 1.2 foe, compared with the observed energy of 1.4 +/- 0.4 foe. It is shown that, and why, the shock wave starts only after some delay.
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