Superfluidity inβ-Stable Neutron Star Matter

Proton and Neutron Superfluidity in β-stable Neutron Star Matter

We investigate the effect of a microscopic three-body force on the proton and neutron superfluidity in the 1S0 channel in β-stable neutron star matter. It is found that the three-body force has only a small effect on the neutron 1S0 pairing gap, but it suppresses strongly the proton 1S0 superfluidity in β-stable neutron star matter. PACS numbers: 26.60.+c,21.65.+f, 21.30.Fe

Superfluidity in Neutron Star Matter

Rapid cooling of the neutron star in Cassiopeia A triggered by neutron superfluidity in dense matter.

We propose that the observed cooling of the neutron star in Cassiopeia A is due to enhanced neutrino emission from the recent onset of the breaking and formation of neutron Cooper pairs in the (3)P(2) channel. We find that the critical temperature for this superfluid transition is ≃0.5×10(9) K. The observed rapidity of the cooling implies that protons were already in a superconducting state wit...

0 Dispersive effects in neutron matter superfluidity

The explicit energy dependence of the single particle self-energy (dispersive effects), due to short range correlations, is included in the treatment of neutron matter superfluidity. The method can be applied in general to strong interacting fermion systems, and it is expected to be valid whenever the pairing gap is substantially smaller than the Fermi kinetic energy. The results for neutron ma...

Semiclassical Approximation to Neutron Star Superfluidity Corrected for Proximity Effects

The inner crust of a neutron star is a superfluid and inhomogeneous system, consisting of a lattice of nuclei immersed in a sea of neutrons. We perform a quantum calculation of the associated pairing gap and compare it to the results one obtains in the Local Density Approximation (LDA). It is found that the LDA overestimates the spatial dependence of the gap, and leads to a specific heat of the...