Magnetorotational Instability in Core-Collapse Supernovae
Abstract
We discuss the relevance of the magnetorotational instability (MRI) in core-collapse supernovae (CCSNe). Our recent numerical studies show that in CCSNe, the MRI is terminated by parasitic instabilities of the Kelvin-Helmholtz type. To determine whether the MRI can amplify initially weak magnetic fields to dynamically relevant strengths in CCSNe, we performed three-dimensional simulations of a region close to the surface of a differentially rotating proto-neutron star in non-ideal magnetohydrodynamics with two different numerical codes. We find that under the conditions prevailing in proto-neutron stars, the MRI can amplify the magnetic field by (only) one order of magnitude. This severely limits the role of MRI channel modes as an agent amplifying the magnetic field in proto-neutron stars starting from small seed fields.
Cite
@article{arxiv.1707.00983,
title = {Magnetorotational Instability in Core-Collapse Supernovae},
author = {Tomasz Rembiasz and Martin Obergaulinger and Jérôme Guilet and Pablo Cerdá-Durán and Miguel-Ángel Aloy and E. Müller},
journal= {arXiv preprint arXiv:1707.00983},
year = {2017}
}
Comments
Proceedings in Acta Physica Polonica B, Proceedings Supplement, Vol. 10, No. 2, p.361, 4 pages, 1 figure