Neutrino transport and hydrodynamic stability of rotating proto-neutron stars

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.

arXiv comment6 pages. Accepted for publication in A&A

References in corpus (19)

• Evolution of Protoneutron Stars
• The Magnetorotational Instability in Core Collapse Supernova Explosions
• Relativistic simulations of rotational core collapse. II. Collapse dynamics and gravitational radiation
• Core-Collapse Simulations of Rotating Stars
• Viscosity and Rotation in Core-Collapse Supernovae
• The Spin Periods and Rotational Profiles of Neutron Stars at Birth
• Towards Gravitational Wave Signals from Realistic Core Collapse Supernova Models
• Ledoux-Convection in Protoneutron Stars --- a Clue to Supernova Nucleosynthesis?
• Multi-Dimensional Radiation/Hydrodynamic Simulations of Protoneutron Star Convection
• The Interplay Between Protoneutron Star Convection and Neutrino Transport in Core Collapse Supernovae
• The Core-Collapse Supernova with "Non-Uniform" Magnetic Fields
• Mean-field dynamo action in protoneutron stars
• Gravitational Waves from Stellar Collapse: Correlations to Explosion Asymmetries
• Protoneutron star dynamos and pulsar magnetism
• Hydromagnetic instabilities in protoneutron stars
• Nonaxisymmetric Magnetorotational Instability in Proto-Neutron Stars
• Convective instability in proto-neutron stars
• Anisotropic convection in rotating proto-neutron stars
• Asymmetry of Strange Sea in Nucleons