On the reconstruction of a magnetosphere of pulsars nearby the light cylinder surface

A mechanism of generation of a toroidal component of large scale magnetic field, leading to the reconstruction of the pulsar magnetospheres is presented. In order to understand twisting of magnetic field lines, we investigate kinematics of a plasma stream co-rotating in the pulsar magnetosphere. Studying an exact set of equations describing the behavior of relativistic plasma flows, the increment of the curvature drift instability is derived, and estimated for I-second pulsars. It is shown that a new parametric mechanism is very efficient and it can explain rotation energy pumping in the pulsar magnetospheres.