Magnetorotational Instability in Proto-Neutron Stars

Details Magnetorotational Instability in Proto-Neutron Stars Magnetorotational Instability in Proto-Neutron Stars

Jun 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aspc..362..117m&link_type=abstract

The Seventh Pacific Rim Conference on Stellar Astrophysics, ASP Conference Series, Vol. 362, Proceedings of the conference held

Astronomy and Astrophysics

Astrophysics

Scientific paper

We investigate the stability of differentially rotating, magnetized proto-neutron stars (PNSs). We find that magnetorotational instability can grow even in stably stratified layers of PNSs if the wavevectors of unstable modes are parallel to the restoring force by thermal and leptonic buoyancy oscillation. The typical growth time of MRI (2π/Ω≃ 100 msec) would be much shorter than the cooling time of PNSs. The nonlinear evolution of MRI could amplify the magnetic fields and drive MHD turbulence in PNSs and this may lead to enhancement of the neutrino luminosity.

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