Neutrino energy equilibration models

Details Neutrino energy equilibration models Neutrino energy equilibration models

Jul 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...239..271t&link_type=abstract

Astrophysical Journal, Part 1, vol. 239, July 1, 1980, p. 271-283. Research supported by the U.S. Department of Energy

Astronomy and Astrophysics

Astrophysics

6

Gravitational Collapse, Magnetohydrodynamics, Neutrinos, Stellar Models, Stellar Radiation, Supernovae, Energy Spectra, Equilibrium Equations, Fokker-Planck Equation, Monte Carlo Method, Transport Properties

Scientific paper

Neutrino energy equilibration by neutrino-electron scattering is studied in four physical models, whose temperatures and densities are representative of stellar collapse conditions when electron scattering may be important. Results of Monte Carlo simulations are presented as data against which approximate transport methods may be tested. The neutrino thermalization rate is initially rapid and approximately exponential, and gradually decreases to slow approach to equilibrium, suggesting the possibility of using a relaxation scheme to approximate the energy equilibration. However, when these results are compared with Fokker-Planck and thermal relaxation algorithms of the kind that have been widely employed in supernova calculations, substantial discrepancies are found. Attempts to recalibrate these approximations yielded reasonable agreement with Monte Carlo results only over relatively restricted temperature and density conditions. These results imply that more sophisticated neutrino energy-equilibration approximations are necessary in order to accurately and efficiently treat supernova core collapse. Directions toward such improved approximations are suggested, and detailed Monte Carlo data are provided against which to test new approaches.

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