Proton superfluidity in neutron-star matter

Physics – Nuclear Physics

Scientific paper

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Scientific paper

We present a microscopic investigation of isotropic proton superfluidity in neutron-star matter, in the framework of the method of correlated basis functions. In the absence of polarization effects, 1S0 proton pairing is found to be considerably weaker than 1S0 neutron pairing, as measured by the peak value of the gap ΔkFN at the Fermi surface with respect to the Fermi wave number kFN of the nucleon component in question. The difference in proton and neutron gaps at the same Fermi wave number is a reflection of the difference in the dispersive effect of the neutron-star medium on a proton as compared to a neutron (difference in effective masses). The proton gap ΔkFp is still sizeable, with a peak value of some 0.6-0.9 MeV occuring at neutron-star densities near that of ordinary nuclear matter. Isotropic proton superfluidity (superconductivity!) is thus expected to prevail over a shell of considerable extent in the interior of a neutron star of ``typical'' mass, temperature, magnetic field and rotational frequency.
Research supported in part by the National Science Foundation under Grant No. GP-22564.

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