Abstract
The timescale of deleptonization by neutrino loss and associated contraction of a proto-neutron star is short compared to the time it takes to propagate a shock through the helium core of a massive star, and so the deleptonization phase does not occur in the vacuum of space, but within the supernova ambiance, whether or not there has been a successful explosion. Dynamical nonaxisymmetric instabilities (NAXI) are predicted for sufficiently strongly differentially rotating proto-neutron stars. Some modes are unstable for small values of the ratio of rotational kinetic energy to binding energy, T/|W| ≳ 0.01. The NAXI are likely to drive magnetoacoustic waves into the surrounding time-dependent density structure. These waves represent a mechanism of the dissipation of the free energy of differential rotation of the proto-neutron star, and the outward deposition of this energy may play a role in the supernova explosion process. We estimate the power produced by this process and the associated timescale and discuss the possible systematics of the deleptonization phase in this context. A likely possibility is that the proto-neutron star will spin down through these effects before deleptonization and produce substantial but not excessive energy input.
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