SUPERFLUIDITY OF ELECTRONS AND AN EFFECT OF THE HALL DRIFT ON THE MAGNETOTHERMAL EVOLUTION OF NEUTRON-STARS

The evolution of the magnetic field in the core of a neutron star is i nvestigated with allowance for the star's cooling. One of the possible models of pre-plasma with electrons in a superfluid state is analyzed . Superfluidity in such a plasma results in the fact that even in a ma gnetized plasma, the magnetic field does not affect the orthogonal com ponent of the electrical resistivity tenser. Nevertheless, the presenc e of a large Hall's component leads to a strong drift of the magnetic field. For the fields greater than or equal to 10(13) G, this drift ma y fundamentally change the field geometry and accelerate its dissipati on. The characteristic time of the field's decay is about 5 x 10(7) yr . The Joule heating significantly slows down the star's cooling, espec ially at late evolutionary stages.