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

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dc.creatorWheeler, J. Craig
dc.creatorAkiyama, Shizuka
dc.date2006-09-26
dc.date.accessioned2026-07-07T10:23:41Z
dc.date.available2026-07-07T10:23:41Z
dc.descriptionThe 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.
dc.description15 pages, 1 figure, accepted for publication in the Astrophysical Journal
dc.identifierhttps://arxiv.org/abs/astro-ph/0609717
dc.identifierhttp://arxiv.org/abs/astro-ph/0609717
dc.identifierAstrophys.J.654:429-434,2006
dc.identifierdoi:10.1086/509111
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/175922
dc.subjectAstrophysics
dc.titleDe-leptonization and Non-Axisymmetric Instabilities in Core Collapse Supernovae
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