Magnetic fields modify bulk viscous dissipation in post-merger neutron star matter by altering direct and modified Urca rates at finite temperature beyond the Fermi surface approximation.
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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.
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Thermal and Magnetic effects on Bulk Viscosity in Binary Neutron Star Mergers
Magnetic fields modify bulk viscous dissipation in post-merger neutron star matter by altering direct and modified Urca rates at finite temperature beyond the Fermi surface approximation.
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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.