Statistics – Computation
Scientific paper
Jun 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26as...78..375j&link_type=abstract
Astronomy and Astrophysics Supplement Series (ISSN 0365-0138), vol. 78, no. 3, June 1989, p. 375-397.
Statistics
Computation
68
Computerized Simulation, Gravitational Collapse, Monte Carlo Method, Neutrino Beams, Supernova Remnants, Computational Astrophysics, Electron Energy, Elementary Particles, Stellar Spectra
Scientific paper
Based on a hydrodynamical model of stellar collapse, spectra and luminosities of neutrinos of various flavors are computed by means of a direct Monte Carlo simulation of neutrino transport. It is shown that local emission and absorption in shocked mater dominates the neutrino flux for at least several tenths of a second after core bounce. The average energy of electron neutrinos drops from about 10 MeV shortly after core bounce to about 8 MeV within 30 msec. Electron antineutrinos leave the star with a mean energy of 14 MeV, while muon and tauon neutrinos have 16-17 MeV at these early stages of the protoneutron star cooling. The typical time scales for stationary flux patterns to develop in the shocked stellar regions are less than 1 msec for electron neutrinos and about 3 to 4 msec for muon and tauon neutrinos.
Hillebrandt Wolfgang
Janka H.-Th.
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