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

Abstract

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.

Efficiency of the centrifugally induced curvature drift instability in AGN winds

“…Even if the field lines have initially a very small curvature, this curvature might cause a drifting process of plasma, which priduces to the CDI. Osmanov et al (2008a) considered the two-component relativistic plasma in studying the role of the centrifugal acceleration in the curvature drift instability for pulsar magnetospheres. The investigation demonstrated that the growth rate was higher than pulsar Article published by EDP Sciences spin-down rates by many orders of magnitude, which implied that the CDI was highly efficient.…”

“…To investigate the twisting process of magnetic field lines due to the CDI, we apply the method developed by Osmanov et al (2008a) and Osmanov et al (2008b) to AGN winds.…”

Dynamical feedback of the curvature drift instability on its saturation process

“…Therefore, the produced electric field should also be considered in Eq. (1) as the next term to be approximated (Osmanov et al 2008).…”

“…Then, by taking into account the formula 1 2π e iNϕ dϕ = δ N,0 , preserving only the leading terms of Eq. (19), and also taking into account that the beam components exceed the corresponding plasma terms by many orders of magnitude, one derives the dispersion relation for the CDI (Osmanov et al 2008)…”

“…Therefore, the process of generating the toroidal component, B r (of the order of B 0 ), requires an additional energy supply, which can be extracted from the pulsar rotational energy. We have already shown that the rotational energy pumping into the drift modes can be implemented by the "parametric" instability (Osmanov et al 2008). This mechanism is called parametric, because the effect is caused by the relativistic centrifugal force, which, as a parameter, changes in time and induces the instability.…”