Abstract
If, as current numerical models show, neutrinos get trapped and become degenerate in the central region of collapsing stellar cores, then they should significantly contribute to their shear viscosity. The magnitude of neutrino viscosity (approx.10/sup 11/ cm/sup 2/ s/sup -1/) is such that it would tend to make a fast rotating stellar core stable beyond the point of bifurcation. The bulk viscosity of such systems is also found to be big, and of the same order of magnitude. The above effects, along with thermal conduction, will tend to damp out acoustical waves generated in a collapsing stellar core after its hydrodynamic bounce.
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