Transport properties of neutrinos in stellar collapse. II - Shear viscosity, heat conduction, and diffusion

Details Transport properties of neutrinos in stellar collapse. II - Shear viscosity, heat conduction, and diffusion Transport properties of neutrinos in stellar collapse. II - Shear viscosity, heat conduction, and diffusion

Jul 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...136...74v&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 136, no. 1, July 1984, p. 74-80. Research supported by the Nederlandse Organis

Statistics

15

Gravitational Collapse, Neutrinos, Stellar Cores, Conductive Heat Transfer, Diffusion Coefficient, Elementary Particle Interactions, Entropy, Fermi-Dirac Statistics, Irreversible Processes, Mean Free Path, Relativistic Plasmas, Stellar Evolution, Transport Properties, Viscosity

Scientific paper

Within the context of relativistic kinetic theory we develop a framework for the calculation of transport properties of neutrinos in stellar collapse. Taking into account both scattering and absorption of the neutrinos, we calculate for arbitrary neutrino degeneracy the transport coefficients characterizing the irreversible heat and diffusion flows as well as the viscous phenomena. Previous results, obtained separately for different physical regimes, are recovered and placed into a single perspective. We assess the relative importance of the various dissipative phenomena by considering their entropy production, and conclude that, depending on degeneracy, heat conduction and diffusion are the dominant dissipative modes. Under favorable conditions, conduction by nondegenerate neutrinos may lead to non-negligible heating on dynamical time scales. Nevertheless, it is not likely to provide the shock strengthening deemed necessary to produce a supernova.

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