CONVECTION IN THE CORES OF NEUTRON-STARS

Explicit expressions for the superadiabatic temperature gradient in the interiors of neutron star are derived. We consider the case without neutron superfluidity and the case with strong neutron superfluidity. Convection in the core of a neutron star becomes possible if die thermal fluxes are directed from the center outward and cause variations in temperature with the local scale not exceeding several kilometers. Convection may arise in the early stages of die evolution of the star [t less than or similar to (1 - 10(3)) years] prior to the temperature relaxation. This effect was not previously taken into account in calculations of neutron-star cooling.