Ferromagnetism of dense matter and magnetic properties of neutron stars

Abstract

Possible consequences of ferromagnetic transition in dense matter suggested recently by Kutschera and W{ó}jcik, for the magnetic properties of neutron stars, are studied. Specific model of dense matter, in which a small admixture of protons is completely polarized due to their interaction with neutrons, is considered. Magnetic field of neutron stars with a ferromagnetic core is calculated within the framework of general relativity. Two types of boundary conditions at the ferromagnetic core edge are considered, corresponding to normal and superconducting liquid envelope, respectively. Numerical results for the neutron star magnetic dipole moment are confronted with pulsar timing. To be consistent with observations, ferromagnetic cores surrounded by a non-superconducting envelope, should consist of weakly ordered ferromagnetic domains. If domains are highly ordered, ferromagnetic core should be screened by a superconducting envelope.

8 pages, Latex, uses l-aa.sty, epsf.tex. Two figures, fig1.eps, fig2.eps. To be published in Astronomy and Astrophysics

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• Coexistence phase of ${}^1{S}_0$ and ${}^3{P}_2$ superfluids in neutron stars
• Neutrino mean free path and in-medium nuclear interaction
• Topological defects at the boundary of neutron ${}^3{P}_2$ superfluids in neutron stars