2006/10/02 by Youhei Masada, Takayoshi Sano, Kazunari Shibata · 2 citations
Physics and Astronomy · #Angular momentum #Astrophysics #Astrophysics and Star Formation Studies #Classical mechanics #Gamma-ray bursts and supernovae #Instability #Magnetohydrodynamics #Magnetorotational instability #Mechanics #Neutrino #Neutron star #Nuclear physics #Physics #Plasma #Pulsars and Gravitational Waves Research #Stars #Supernova #Toroid #astro-ph
paper · pdf · doi:10.1086/509799
published as Astrophys.J.655:447-457,2007 · Accepted for publication in ApJ, 24 pages,6 figures
arxiv created 2006/10/02 · openalex publication_date 2007/01/20 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Neutrino radiation takes a major role in the momentum, heat, and lepton transports in proto-neutron stars (PNSs). These diffusive processes affect the growth of the magnetorotational instability (MRI) in PNSs. We perform a local linear analysis for the axisymmetric and nonaxisymmetric MRI including the effects of neutrino transport and ohmic dissipation. We find that the MRI can grow even in the multidiffusive situations that are realized in neutrino-loaded PNSs. When the toroidal magnetic component dominates over the poloidal one, nonaxisymmetric MRI modes grow much faster than axisymmetric modes. These results suggest the importance of the nonaxisymmetric MRI in PNSs. Thus, understanding the three-dimensional nonlinear evolution of the MRI is necessary for revealing the explosion mechanism of core-collapse supernovae.