Abstract
In this paper, we consider the relativistic effects of rotation in the magnetospheres of γ-ray pulsars. The paper reviews the progress achieved in this field during the last three decades. For this purpose, we examine the direct centrifugal acceleration of particles and the corresponding limiting factors: the constraints due to the curvature radiation and the inverse Compton scattering of electrons against soft photons. Based on the obtained results, the generation of parametrically excited Langmuir waves and the corresponding Landau–Langmuir centrifugal drive are studied.
Highlights
One of the fundamental problems of γ-ray pulsar astrophysics is the generation of VHE emission
Where the slow down rate is normalized by the typical value for normal period pulsars, and we have taken into account that the moment of the inertia of a sphere is expressed as I = 2MnsR2/5, where Mns denotes the neutron star’s mass, R 106 cm is its radius, and M 2 × 1033 g is the solar mass
The corresponding problem, but in a special relativistic case, was studied in [24], where the authors considered a gedanken experiment: a bead freely sliding on a rotating wire, and studied the particle’s dynamics
Summary
One of the fundamental problems of γ-ray pulsar astrophysics is the generation of VHE emission. Where the slow down rate is normalized by the typical value for normal period pulsars (with a period of the order of one second) , and we have taken into account that the moment of the inertia of a sphere is expressed as I = 2MnsR2/5, where Mns denotes the neutron star’s mass, R 106 cm is its radius, and M 2 × 1033 g is the solar mass It is clear from the aforementioned expression that the slowing down of pulsar’s rotation provides enormous power, which might be even higher for millisecond pulsars. A rather different mechanism of acceleration that might take place in the LC zone was proposed by Gold [18,19], who suggested that an extremely strong magnetic field forces particles to slide along the field lines, which are the trajectories of particles in the rotating frame of reference. We apply the model of centrifugal acceleration to the wellknown Crab and Vela pulsars and normal period pulsars, and in Section 3, we outline the obtained results
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