English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We investigate the evolution of the chiral magnetic instability in aprotoneutron star and compute the resulting magnetic power and helicityspectra. The instability may act during the early cooling phase of the hotprotoneutron star after supernova core collapse, where it can contribute to thebuildup of magnetic fields of strength up to the order of $10^{14}$ G. Themaximal field strengths generated by this instability, however, dependconsiderably on the temperature of the protoneutron star, on densityfluctuations and turbulence spectrum of the medium. At the end of the hotcooling phase the magnetic field tends to be concentrated around thesubmillimeter to cm scale, where it is subject to slow resistive damping.

Chiral Magnetic Effect in Protoneutron Stars and Magnetic Field Spectral Evolution