2008MNRAS.383.1007O

A mechanism of the 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 behaviour of relativistic plasma flows, the increment of the curvature drift instability is derived, and estimated for 1-s pulsars. It is shown that a new parametric mechanism is very efficient and it can explain rotation energy pumping in the pulsar magnetospheres.