A Model for unusual pulsed X - ray emission from PSR J 1119 - 6127

We propose a model, which naturally explains an unusual thermal X-ray emission, observed from PSR J1119-6127. The model is based on the assumption that the pulsar magnetic field near the stellar surface differs significantly from the pure dipole field. We show that the structure and curvature of the field lines can be of the kind that allows the pair creation in the closed field line region. The created pairs propagate along the closed field lines and heat the stellar surface beyond the local poles. It is demonstrated that such a configuration can be easily realized. Thermal X-ray emission seems to be a quite common feature of the radio pulsars. On the other hand characteristics of such radiation allows us to get a lot of information about the polar cap region of the pulsars. Standard model of the radio pulsars assumes that there exists the Inner Acceleration Region (IAR) 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. Consequently, outstreaming particles generate the magnetospheric (radio and high-frequency) emission while the the backstreaming particles heat the surface and provide necessary energy for the thermal emission. In such a scenario X-ray diagnostics seems to be an excellent method to get insight into the most intriguing regain of the neutron star. The black body fit allows us to obtain directly the bolometric size (Abol) and temperature (Ts) of the polar cap. In most casesAbol is much less than the conventional polar cap area. It can be easily explained by assuming that the surface magnetic field of pulsars differs significantly from the pure dipole one. Then, one can estimate an actual surface magnetic field by the magnetic flux conservation law as b = Abol/Apc = Bd/Bs. Here Bd = 2×10 12 (