Energy Gap in Neutron-Star Matter

Superfluidity in Neutron Star Matter

Isospin-rich nuclei in neutron star matter

Stability of nuclei beyond the drip lines in the presence of an enveloping gas of nucleons and electrons, as prevailing in the inner crust of a neutron star, is studied in the temperature-dependent Thomas-Fermi framework. A limiting asymmetry in the isospin space beyond which nuclei cannot exist emerges from the calculations. The ambient conditions like temperature, baryon density and neutrino ...

Kaon Condensation in Proto-Neutron Star Matter

We study the equation of state of kaon-condensed matter including the effects of temperature and trapped neutrinos. Several different field-theoretical models for the nucleon-nucleon and kaon-nucleon interactions are considered. It is found that the order of the phase transition to a kaon-condensed phase, and whether or not Gibbs’ rules for phase equilibrium can be satisfied in the case of a fi...

Strangeness Nucleation in Neutron Star Matter

We study the transition from npe-type nuclear matter (consisting of neutrons, protons, and electrons) to matter containing strangeness, using a Walecka-type model predicting a first-order kaon-condensate phase transition. We examine the free energy of droplets of K-matter as the density, temperature, and neutrino fraction are varied. Langer nucleation rate theory is then used to approximate the...

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