On the magnetohydrodynamic modelling of the Crab nebula radio emission

In recent years, it has become a well-established paradigm that many aspects of the physics of Pulsar Wind Nebulae can be fully accounted for within a relativistic magnetohydrodynamic description. Numerical simulations have proven extremely successful in reproducing the X-ray morphology of the Crab nebula, down to very fine detail. Radio emission, instead, is currently one of the most obscure aspects of the physics of these objects, and one that holds important information about pulsar properties and their role as antimatter factories. Here, we address the question of radio emission morphology and integrated spectrum from the Crab nebula, by using for the first time an axisymmetric dynamical model with parameters chosen to best reproduce its X-ray morphology. Based on our findings we discuss constraints on the origin of the radio emitting particles.