Neutral currents and neutrino Comptonization in high-temperature, nuclear matter

Details Neutral currents and neutrino Comptonization in high-temperature, nuclear matter Neutral currents and neutrino Comptonization in high-temperature, nuclear matter

Nov 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...233..961s&link_type=abstract

Astrophysical Journal, Part 1, vol. 233, no. 3, Nov. 1, 1979, p. 961-973.

Astronomy and Astrophysics

Astrophysics

1

Astrophysics, Compton Effect, Energy Transfer, Neutrinos, Nucleons, Cross Sections, Electron Scattering, Gravitational Collapse, High Temperature, Supernovae

Scientific paper

The paper deals with the effect of neutrino Comptonization, by which energy is exchanged between a hot, dense nucleon gas and a neutrino gas via Compton scattering, on the final spectrum of the neutrinos. The diffusion equation which governs Comptonization is derived and integrated to get energy exchange rates. The rates and other reasonable assumptions are used to develop rough criteria by which it is possible to determine whether or not Comptonization will be important in a gas of given temperature and density. A crude model transport equation is given which accounts for several of the processes that cause energy exchange between neutrinos and the gas and calculate spectra. It is concluded that Comptonization can have a marked effect on neutrino spectra whenever our rough criteria are satisfied. When applied to conditions likely to occur during stellar core collapse, it is found that Comptonization will be important for densities in excess of 10 to the 13th power g/cu cm and temperatures in a wide range about 10 to the 11th power K in a free nucleon gas. A dominance of high-A nuclei, however, will make Comptonization less important than electron scattering, typically, due to the larger number of electrons per baryon Ye necessary to cancel the charge of the protons found in the nuclei.

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