Magnetic Reconnection in the Accretion-Disc Corona of a Compact Star

We propose a new model for the magnetosphere of a rotating compact star with an accretion disc in the case where the magnetic axis of the star is not perpendicular to the rotation axis. We estimate the values of the magnetic field and its gradient in the accretion-disc corona. Then these estimates are used as the initial data for developing an analytical model of a reconnecting current sheet and evaluating its parameters and the energy release in the accretion disc corona. It is shown that the magnetic reconnection can contribute essentially to the X-ray radiation observed from compact stars.