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Title: MAGNETOHYDRODYNAMIC TURBULENCE POWERED BY MAGNETOROTATIONAL INSTABILITY IN NASCENT PROTONEUTRON STARS

Magnetorotational instability (MRI) in a convectively stable layer around the neutrinosphere is simulated by a three-dimensional model of a supernova core. To resolve MRI-unstable modes, a thin layer approximation considering only the radial global stratification is adopted. Our intriguing finding is that the convectively stable layer around the neutrinosphere becomes fully turbulent due to the MRI and its nonlinear penetration into the strongly stratified MRI-stable region. The intensity of the MRI-driven turbulence increases with magnetic flux threading the core, but is limited by the free energy stored in the differential rotation. The turbulent neutrinosphere is a natural consequence of rotating core-collapse and could exert a positive impact on the supernova mechanism.
Authors:
 [1] ;  [2] ;  [3]
  1. Department of Computational Science, Kobe University, Kobe 657-8501 (Japan)
  2. Division of Theoretical Astronomy, National Astronomical Observatory of Japan, Tokyo 181-8588 (Japan)
  3. Faculty of Science, Department of Applied Physics, Fukuoka University, Fukuoka 814-0180 (Japan)
Publication Date:
OSTI Identifier:
22364712
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal Letters; Journal Volume: 798; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; APPROXIMATIONS; COMPUTERIZED SIMULATION; COSMIC NEUTRINOS; FREE ENERGY; LAYERS; MAGNETIC FLUX; MAGNETOHYDRODYNAMICS; NONLINEAR PROBLEMS; ROTATION; STAR MODELS; STRATIFICATION; SUPERNOVAE; THIN FILMS; THREE-DIMENSIONAL CALCULATIONS; TURBULENCE