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arXiv · 0704.3162

Neutrino transport and hydrodynamic stability of rotating proto-neutron stars

V. Urpin
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Abstract

We consider stability of differentially rotating non-magnetic proto-neutron stars. When neutrino transport is efficient, the star can be subject to a diffusive instability that can occur even in the convectively stable region. The instability arises on the time-scale comparable to the time-scale of thermal diffusion. Hydrodynamic motions driven by the instability can lead to anisotropy in the neutrino flux since the instability is suppressed near the equator and rotation axis.

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V. Urpin. 2007-04-24. Neutrino transport and hydrodynamic stability of rotating proto-neutron stars. https://doi.org/10.1051/0004-6361%3A20066258

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