Abstract
The Crab Nebula is powered by the central pulsar. The appearance of lumpy and patchy structures within the nebula results from inhomogeneous distributions of magnetic field and of relativistic electron density. In this paper, we focus on the primary origin of inhomogeneous magnetic field structures. For that purpose, we develop a theoretical model for a two-dimensional propagation of Alfvenic perturbations within the equatorial plane of an axisymmetric relativistic magnetohydrodynamic (RMHD) wind embedded with a spiral magnetic field caused by the rotation of a central source. We obtain analytical solutions within the entire frequency range for asymptotic Alfvenic perturbations at a large radial distance r
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