Neutrino transport and hydrodynamic stability of rotating proto-neutron stars

Details Neutrino transport and hydrodynamic stability of rotating proto-neutron stars Neutrino transport and hydrodynamic stability of rotating proto-neutron stars

2007-04-24

arxiv.org/abs/0704.3162v1

Astronomy and Astrophysics

Astrophysics

6 pages. Accepted for publication in A&A

Scientific paper

10.1051/0004-6361:20066258

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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