Pion Condensation and Magnetism in Neutron Stars

Details Pion Condensation and Magnetism in Neutron Stars Pion Condensation and Magnetism in Neutron Stars

Oct 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002pthph.108..689t&link_type=abstract

Progress of Theoretical Physics, Vol. 108, No. 4, pp. 689-701

Physics

5

Scientific paper

The linear σ model (LσM) suggests that the nuclear matter exhibits a phase transition to a pion-condensed ferromagnetic state at a few times the normal nuclear matter density. Extending the naïve LσM so as to reproduce the known bulk properties of nuclear matter around saturation, the equation of state of neutron star matter is constructed and used as an input for solving the Tolman-Oppenheimer-Volkoff equation. It is found that there exist gravitationally stable solutions to this equation. These solutions can model neutron stars with a maximal dipole magnetic field of O(1014 - 1015 G).

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