Abstract
We propose a model that explains the observed thermal X-ray emission from the surface of neutron stars (pulsars). Characteristics of such radiation allow us to get a lot of in-formation about the polar cap region of the pulsars, where the thermal X-ray radiation is believed to be generated. The model requires existence of a strong and non-dipolar surface magnetic field. We provide a numerical formalism for modeling such structures at the stellar surface and calculating the basic parameters that can be fitted to the observational data. We assume that the source of the pulsar activity is associated with the region just above the polar cap where the electric field has a component along the magnetic field lines. The particles (electrons and positrons) are accelerated in both directions: outward and toward the stellar surface. The back-streaming particles heat the surface and provide necessary energy for the thermal emission. We discuss various possible configurations of the surface magnetic field and demonstrate that the model naturally allows interpretation of observations.
