Transport properties of neutrinos in stellar collapse. I Bulk viscosity of collapsing stellar cores

Details Transport properties of neutrinos in stellar collapse. I Bulk viscosity of collapsing stellar cores Transport properties of neutrinos in stellar collapse. I Bulk viscosity of collapsing stellar cores

Aug 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...125...93v&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 125, no. 1, Aug. 1983, p. 93-100. Research supported by the Nederlandse Organi

Astronomy and Astrophysics

Astrophysics

8

Elementary Particle Interactions, Gravitational Collapse, Neutrinos, Stellar Cores, Transport Properties, Viscosity, Electron Capture, Kinetic Equations, Relativistic Plasmas, Thermodynamic Properties

Scientific paper

A detailed kinetic theory calculation is presented for the bulk viscosity due to neutrinos in interaction with a material medium representative of a collapsing stellar core. The general theory of bulk viscous dissipation in a relativistic imperfect fluid is outlined. In stellar collapse, the bulk viscosity arises primarily from neutrino absorption by neutrons and electron capture on protons. Assuming these reactions to be in local chemical equilibrium, the linearized relativistic neutrino transport equation is solved for the case of bulk viscous dissipation. Owing to the equilibrium constraint, the solution is determined by a single absorption parameter. The final result for the bulk viscosity coefficient is valid for arbitrary neutrino degeneracy and is shown to comprise a number of previously published expressions. In spite of its large numerical value (about 10 to the 24th g/cm s), the bulk viscosity generates negligible pressure or entropy enhancement during the infall epoch of the core. It is estimated to be effective only on a time scale of the order of 1s.

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