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We study the effects of heat blanketing envelopes of neutron stars on theircooling. To this aim, we perform cooling simulations using newly constructedmodels of the envelopes composed of binary ion mixtures (H--He, He--C, C--Fe)varying the mass of lighter ions (H, He or C) in the envelope. The results arecompared with those calculated using the standard models of the envelopes whichcontain the layers of lighter (accreted) elements (H, He and C) on top of theFe layer, varying the mass of accreted elements. The main effect is that thechemical composition of the envelopes influences their thermal conductivityand, hence, thermal insulation of the star. For illustration, we apply theseresults to estimate the internal temperature of the Vela pulsar and to studythe cooling of neutron stars of ages of 0.1 - 1 Myr at the photon coolingstage. The uncertainties of the cooling models associated with our poorknowledge of chemical composition of the heat insulating envelopes stronglycomplicate theoretical reconstruction of the internal structure of coolingneutron stars from observations of their thermal surface emission.

Cooling of neutron stars with diffusive envelopes