Permanent mean spin source of the chiral magnetic effect in neutron stars

Abstract

We suggest the generalization of the Anomalous Magneto-Hydro-Dynamics (AMHD) in the chiral plasma of a neutron star (NS) accounting for the mean spin in the ultrarelativistic degenerate electron gas within the magnetized NS core as a continuing source of the chiral magnetic effect. Using the mean field dynamo model generalized in AMHD, one can obtain the growth of a seed magnetic field up to $10^{18}\text{G}$ for an old non-superfluid NS at its neutrino cooling era $t<10^6\text{yr}$, while neglecting any matter turbulence within its core and assuming the rigid NS rotation. The application of the suggested approach to the evolution of magnetic fields observed in magnetars, $B\sim 10^{15}\text{G}$, should be self-consistent with all approximations used in the suggested laminar dynamo, at least, up to the jumps of growing fields.

arXiv comment15 pages, 9 eps figures, JCAP latex style; title is modified, minimal changes in the text; version published in JCAP

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• Probing ALP-photon couplings in Neutron Stars: Scalar versus pseudoscalar cases
• Magnetic helicity in rotating neutron stars