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
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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.
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QED scattering amplitudes in a chiral medium with constant μ5 and b0 exhibit resonant behavior in multiple processes, with computed rates for 1→2 processes determining widths of fermion and photon states.
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.
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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.