Effect of vacuum polarization by magnetic field on radiative thermal conductivity of surface layers of neutron stars

The radiative Thomsom thermal conductivity is calculated for a non-relativistic no-degenerate plasma of surface layers of neutron stars in a strong magnetic field B with allowance for polarization of electron-positron vacuum. The effect of the magnetic field is significant at b=h#betta#sub(B)/kT > or approximately 2 (#betta#sub(B) being the cyclotron frequency). The vacuum polarization may change the thermal conductivities along and across the magnetic field kappasub(parallel) and kappasub(perpendicular), by several times, the sign of the difference kappasub(parallel)-kappasub(perpendicular) also being changed. The performed calculations are required for constructing the models of X-ray pulsars as well as for investigating various phenomena concerned with heat transfer in surface layers of neutron stars