A numerical method for solving the neutrino Boltzmann equation coupled to spherically symmetric stellar core collapse

Details A numerical method for solving the neutrino Boltzmann equation coupled to spherically symmetric stellar core collapse A numerical method for solving the neutrino Boltzmann equation coupled to spherically symmetric stellar core collapse

Mar 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...405..669m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 405, no. 2, p. 669-684.

Statistics

Computation

83

Boltzmann Transport Equation, Computational Astrophysics, Finite Difference Theory, Gravitational Collapse, Neutrinos, Stellar Cores, Hydrodynamics, Newton-Raphson Method, Radiation Transport, Symmetry

Scientific paper

A numerical method for solving the Boltzmann equation coupled to hydrodynamic flows, a relativistic equation of state, and lepton conservation for fermion transport has been developed. Difficulties encountered in past attempts to solve the neutron Boltzmann equation in stellar cores have been overcome. In particular, the correct diffusion limit for optically thick zones has been obtained without introducing ad hoc factors in the radial transport term. Oscillations in the neutrino distribution function in optically thin zones have been avoided. New numerical techniques for the angular aberration and frequency shift terms have been developed and successfully implemented. In particular, a finite difference representation has been developed for the angular aberration term that can be used with Gaussian quadratures and Bruenn's method has been successfully generated for the frequency shift term.

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