Volume 469, Number 2, July II 2007
|Page(s)||639 - 644|
|Section||Stellar structure and evolution|
|Published online||02 May 2007|
Neutrino transport and hydrodynamic stability of rotating proto-neutron stars
Departament de Fisica Aplicada, Universitat d'Alacant, Ap. Correus 99, 03080 Alacant, Spain e-mail: Vadim.Urpin@uv.es
2 A.F. Ioffe Institute of Physics and Technology and Isaac Newton Institute of Chile, Branch in St. Petersburg, 194021 St. Petersburg, Russia
Accepted: 29 March 2007
Aims.We study the stability of differentially rotating, non-magnetic proto-neutron stars.
Methods.The stability is considered by making use of a linear analysis and taking neutrino transport into account.
Results.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 a time scale that is 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.
Key words: stars: neutron / stars: rotation / stars: supernovae: general / hydrodynamics / instabilities
© ESO, 2007
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