Long-term numerical relativity simulations find that neutron star magnetic fields relax to stable mixed configurations with toroidal energy fraction ≲10% within one Alfvén time after Tayler instability saturation.
Evolution of the magnetic field in neutron stars
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abstract
We propose a general method to self-consistently study the quasistationary evolution of the magnetic field in the cores of neutron stars. The traditional approach to this problem is critically revised. Our results are illustrated by calculation of the typical timescales for the magnetic field dissipation as functions of temperature and the magnetic field strength.
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2026 2verdicts
UNVERDICTED 2representative citing papers
Complete one-loop self-energies computed for the linear sigma model with quarks at finite temperature and magnetic field via Matsubara and Schwinger/Ritus formalisms.
citing papers explorer
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Magnetic field dynamics in isolated neutron stars with an external dipole field
Long-term numerical relativity simulations find that neutron star magnetic fields relax to stable mixed configurations with toroidal energy fraction ≲10% within one Alfvén time after Tayler instability saturation.
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Complete one-loop self-energies of the linear sigma model coupled to quarks at finite temperature and in a magnetic field
Complete one-loop self-energies computed for the linear sigma model with quarks at finite temperature and magnetic field via Matsubara and Schwinger/Ritus formalisms.