Journal
JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
Volume -, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/1475-7516/2016/01/025
Keywords
Magnetohydrodynamics; magnetic fields; neutron stars
Funding
- Helmholtz Alliance for Astroparticle Physics (HAP) - Initiative and Networking Fund of the Helmholtz Association
- Deutsche Forschungsgemeinschaft (DFG) through the Collaborative Research Centre Particles, Strings and the Early Universe [SFB 676]
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We investigate the evolution of the chiral magnetic instability in a protoneutron star and compute the resulting magnetic power and helicity spectra. The instability may act during the early cooling phase of the hot protoneutron star after supernova core collapse, where it can contribute to the buildup of magnetic fields of strength up to the order of 10(14) G. The maximal field strengths generated by this instability, however, depend considerably on the temperature of the protoneutron star, on density fluctuations and turbulence spectrum of the medium. At the end of the hot cooling phase the magnetic field tends to be concentrated around the submillimeter to cm scale, where it is subject to slow resistive damping.
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