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Astrophysics and Space Science manuscript No. (will be inserted by the editor) Alexander Y. Potekhin · Gilles Chabrier · Dmitry G. Yakovlev Heat Blanketing Envelopes and Thermal Radiation of Strongly Magnetized Neutron Stars 6 Received: July 5, 2006 / Accepted: October 31, 2006 0 0 2 Abstract Strong (B ≫ 109 G) and superstrong (B 1 Introduction v 1014 G) magnetic fields profoundly affect many ther- o modynamic and kinetic characteristics of dense plasmas Thermal emission from neutron stars can be used to N in neutron star envelopes. In particular, they produce measure the magnetic field, temperature, and compo- 1 strongly anisotropic thermal conductivity in the neutron sition of neutron-star envelopes, and to constrain the star crust and modify the equation of state and radia- properties of matter under extreme conditions (see, e.g., tive opacities in the atmosphere, which are major in- Yakovlev Pethick 2004; Yakovlev et al. 2005, and ref- 1 gredients of the cooling theory and spectral atmosphere erences therein). To achieve these goals, one should use v models. As a result, both the radiation spectrum and the reliable models of the atmosphere or condensed surface, 4 thermal luminosity of a neutron star can be affected by where the thermal spectrum is formed, and of deeper 1 the magnetic field. We briefly review these effects and layers, which provide thermal insulation of hot stel- 0 demonstrate the influence of magnetic field strength on lar interiors. In these layers, the effects of strong mag- 1 the thermal structure of an isolated neutron star, putting netic fields can be important. In recent years, significant 1 6 emphasis on the differences brought about by the super- progress has been achieved in the theoretical desc