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.
Magnetars and the Chiral Plasma Instabilities
3 Pith papers cite this work. Polarity classification is still indexing.
3
Pith papers citing it
abstract
We propose a possible new mechanism for a strong and stable magnetic field of compact stars due to an instability in the presence of a chirality imbalance of electrons---the chiral plasma instability. A large chirality imbalance of electrons inevitably occurs associated with the parity-violating weak process during core collapse of supernovae. We estimate the maximal magnetic field due to this instability to be of order 10^{18} G at the core. This mechanism naturally generates a large magnetic helicity from the chiral asymmetry, which ensures the stability of the large magnetic field.
citation-role summary
background 1
citation-polarity summary
verdicts
UNVERDICTED 3roles
background 1polarities
background 1representative citing papers
Chiral dynamos grow too slowly and are suppressed by flipping when chirality is pumped gradually, rendering them inefficient in protoneutron stars and barely viable near the electroweak transition.
Time-dependent electric fields in relativistic drifting plasma induce polarization drift that modifies the induced current structure, with quantitative estimates of Hall and polarization contributions provided for the quark-gluon plasma.
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.
-
Inefficiency of chiral dynamos in protoneutron stars and the early universe
Chiral dynamos grow too slowly and are suppressed by flipping when chirality is pumped gradually, rendering them inefficient in protoneutron stars and barely viable near the electroweak transition.
-
Electromagnetic response of a relativistic drifting plasma
Time-dependent electric fields in relativistic drifting plasma induce polarization drift that modifies the induced current structure, with quantitative estimates of Hall and polarization contributions provided for the quark-gluon plasma.