De-leptonization and Non-Axisymmetric Instabilities in Core Collapse Supernovae

Details De-leptonization and Non-Axisymmetric Instabilities in Core Collapse Supernovae De-leptonization and Non-Axisymmetric Instabilities in Core Collapse Supernovae

2006-09-26

arxiv.org/abs/astro-ph/0609717v1

Astrophys.J.654:429-434,2006

Astronomy and Astrophysics

Astrophysics

15 pages, 1 figure, accepted for publication in the Astrophysical Journal

Scientific paper

10.1086/509111

The timescale of de-leptonization by neutrino loss and associated contraction of a proto-neutron star is short compared to the time to progagate a shock through the helium core of a massive star, and so the de-leptonization phase does not occur in the vacuum of space, but within the supernova ambiance whether or not there has been a successful explosion. Dynamical non-axisymmetric 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 de-leptonization phase in this context. A likely possibility is that the proto-neutron star will spin down through these effects before de-leptonization and produce substantial but not excessive energy input.

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