MAGNETOHYDRODYNAMIC TURBULENCE POWERED BY MAGNETOROTATIONAL INSTABILITY IN NASCENT PROTONEUTRON STARS

Journal Article · Thu Jan 01 04:00:00 EST 2015 · Astrophysical Journal Letters

DOI:https://doi.org/10.1088/2041-8205/798/1/L22· OSTI ID:22364712

Masada, Youhei ^[1]; Takiwaki, Tomoya ^[2]; Kotake, Kei ^[3]

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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)

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.

• OSTI ID: 22364712
• Journal Information: Astrophysical Journal Letters, Journal Name: Astrophysical Journal Letters Journal Issue: 1 Vol. 798; ISSN 2041-8205
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
APPROXIMATIONS
COMPUTERIZED SIMULATION
COSMIC NEUTRINOS
FREE ENERGY
LAYERS
MAGNETIC FLUX
MAGNETOHYDRODYNAMICS
NONLINEAR PROBLEMS
ROTATION
STAR MODELS
STRATIFICATION
SUPERNOVAE
THIN FILMS
THREE-DIMENSIONAL CALCULATIONS
TURBULENCE