Higher temperatures enable chiral plasma instability to grow magnetic fields from modest chiral chemical potentials, while CME from density fluctuations produces rapid Joule heating reaching QCD-scale energies in milliseconds to seconds.
Chiral Magnetic Effect in Protoneutron Stars and Magnetic Field Spectral Evolution
3 Pith papers cite this work. Polarity classification is still indexing.
3
Pith papers citing it
abstract
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.
citation-role summary
background 2
citation-polarity summary
verdicts
UNVERDICTED 3roles
background 2polarities
background 2representative citing papers
Chiral magnetic effect generates magnetar-strength dipoles independently of initial net helicity via localized structures on decade timescales.
During chiral plasma instability, excess energy from chiral asymmetry heats the plasma with δT ~ μ5²/T instead of fully building the helical magnetic field.
citing papers explorer
-
Chiral effects and Joule heating in hot and dense matter
Higher temperatures enable chiral plasma instability to grow magnetic fields from modest chiral chemical potentials, while CME from density fluctuations produces rapid Joule heating reaching QCD-scale energies in milliseconds to seconds.
-
Magnetar field dynamics driven by chiral anomalies without magnetic helicity
Chiral magnetic effect generates magnetar-strength dipoles independently of initial net helicity via localized structures on decade timescales.
-
Plasma heating during the chiral plasma instability
During chiral plasma instability, excess energy from chiral asymmetry heats the plasma with δT ~ μ5²/T instead of fully building the helical magnetic field.