Turbulent magnetic field amplification from spiral SASI modes in core-collapse supernovae

We describe the initial implementation of magnetohydrodynamics (MHD) in our astrophysical simulation code \genasis. Then, we present MHD simulations exploring the capacity of the stationary accretion shock instability (SASI) to generate magnetic fields by adding a weak magnetic field to an initially...

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Bibliographic Details
Published in:arXiv.org 2012-03
Main Authors: Endeve, E, Cardall, C Y, Budiardja, R D, Mezzacappa, A
Format: Article
Language:English
Subjects:
Amplification
Collapse
Computational fluid dynamics
Computer simulation
Deposition
Fluid flow
Magnetic fields
Magnetism
Magnetohydrodynamic turbulence
Magnetohydrodynamics
Neutron stars
Stability
Supernovae
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Description
Summary:We describe the initial implementation of magnetohydrodynamics (MHD) in our astrophysical simulation code \genasis. Then, we present MHD simulations exploring the capacity of the stationary accretion shock instability (SASI) to generate magnetic fields by adding a weak magnetic field to an initially spherically symmetric fluid configuration that models a stalled shock in the post-bounce supernova environment. Upon perturbation and nonlinear SASI development, shear flows associated with the spiral SASI mode contributes to a widespread and turbulent field amplification mechanism. While the SASI may contribute to neutron star magnetization, these simulations do not show qualitatively new features in the global evolution of the shock as a result of SASI-induced magnetic field amplification.
ISSN:2331-8422
DOI:10.48550/arxiv.1203.3385