G. Lazzari

Emissivities of neutrinos in neutron star cores.

In this work we consider the role of muons in various URCA processes relevant for neutrino emissions in the core region of neutron stars. The calculations are done for

NUCLEAR EFFECTS ON SUPERFLUID NEUTRON STAR MATTER

\beta

Pinning properties of superfluid vortices in the crust of neutron stars

--stable nuclear matter with and without muons. We find muons to appear at densities

PROTON SUPERFLUIDITY IN NEUTRON STAR MATTER WITH AN EFFECTIVE INTERACTION

\rho = 0.15

Vortex pinning with non-spherical nuclei

fm

Pairing properties of clustered protons in neutron star crusts

^{-3}

Semi-classical description of the neutron superfluid in the inner crust of neutron stars

, slightly around the saturation density for nuclear matter

Specific heat of the superfluid neutron matter in neutron star crusts

\rho_0 =0.16

Specific heat of protons in non-spherical nuclei

fm

HEAT DIFFUSION TIME IN NEUTRON STAR CRUSTS

^{-3}