Neutrino emission from a hot, dense, plane-parallel atmosphere in hydrostatic equilibrium. II - Numerical methods and interaction functions

Details Neutrino emission from a hot, dense, plane-parallel atmosphere in hydrostatic equilibrium. II - Numerical methods and interaction functions Neutrino emission from a hot, dense, plane-parallel atmosphere in hydrostatic equilibrium. II - Numerical methods and interaction functions

Sep 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apjs...50...23s&link_type=abstract

Astrophysical Journal Supplement Series, vol. 50, Sept. 1982, p. 23-37.

Astronomy and Astrophysics

Astronomy

23

Neutrinos, Nuclear Reactions, Particle Emission, Scattering Functions, Stellar Atmospheres, Weak Interactions (Field Theory), Absorptivity, Annihilation Reactions, Antineutrinos, Atmospheric Heating, Black Holes (Astronomy), Electron-Positron Pairs, Entropy, Hydrostatics, Pair Production

Scientific paper

Detailed neutrino and antineutrino emission and absorption coefficients for beta-decay interactions are assembled, along with coefficients for neutrino and antineutrino scattering from protons, neutrons, electrons and positrons, absorption and emission coefficients for neutrino-antineutrino pair emission, and absorption by electron-positron pairs and plasmons. These formulas are presented in a form suitable for use in the neutrino and antineutrino transport equations. A numerical method to solve the problem of a plane-parallel, semiinfinite, static neutrino atmosphere 'heated from below' is described in detail. Explicit relations are given for the entropy of a gas of free electrons, protons, neutrons, positrons, photons, neutrinos, and antineutrinos, and it is shown how these relations can be used to calculate the convective stability criterion discussed elsewhere.

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