Neutrino emission dfrom a hot, dense, plane-parallel atmosphere in hydrostatic equilibrium

Details Neutrino emission dfrom a hot, dense, plane-parallel atmosphere in hydrostatic equilibrium Neutrino emission dfrom a hot, dense, plane-parallel atmosphere in hydrostatic equilibrium

Mar 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982phdt.........4s&link_type=abstract

Ph.D. Thesis Cornell Univ., Ithaca, NY.

Physics

Neutrinos, Particle Interactions, Stellar Atmospheres, Stellar Radiation, Collapse, Differential Equations, Electrons, Flavor (Particle Physics), Muons, Transport Theory, Weak Interactions (Field Theory)

Scientific paper

Neutrino transport appropriate to the core collapse of a massive star is investigated by studying transport in a plane-parallel equilibrium atmosphere. The solution of this problem is numerical and is obtained by finite differencing the exact time-independent transport equation. This equation is an integro-differential equation which has three independent variables, corresponding to depth below the surface, neutrino energy, and neutrino direction cosine. The desired solution is constrained to be in hydrostatic equilibrium with constant gravitational acceleration g, to conserve total energy flux F, and to conserve lepton number flux (or, in the case of three flavored atmospheres, fluxes) N. Two different types of atmosphere are constructed. In the first, only electron neutrinos and antineutrinos are allowed to exist in the atmosphere. In the second, all three flavors of neutrino (electron, mu, and tau) are incorporated. Detailed formulae for the interaction functions necessary to describe electron, mu, and tau neutrino interactions with protons, neutrons, electrons, positrons and plasmons are also presented. Numerical calculations of the emitted spectra and the profiles of various parameters describing the state of the atmosphere for both one and three flavored are presented.

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