Motion of test particles along rotating curved trajectories is considered. The problem is studied both in the laboratory and the rotating frames of reference. It is assumed that the system rotates with the constant angular velocity ω = const. The solutions are found and analyzed for the case when the form of the trajectory is given by an Archimedes spiral. It is found that particles can reach infinity while they move along these trajectories and the physical interpretation of their behaviour is given. The analogy of this idealized study with the motion of particles along the curved rotating magnetic field lines in the pulsar magnetosphere is pointed out. We discuss further physical development (the conserved total energy case, when ω = const) and astrophysical applications (the acceleration of particles in active galactic nuclei) of this theory.
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.
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 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 1s pulsars. It is shown that a new parametric mechanism is very efficient and can explain rotation energy pumping in the pulsar magnetospheres.
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