Time dependent numerical simulations show that the anisotropy of the energy flux and a weak magnetization of the pulsar winds result into formation of the most spectacular features in the central part of the plerions, namely the X‐ray tore and jet‐like outflows. We present the results of such simulations performed by our group. One of the most important conclusions following from this study is the fact that these structures are a direct observational proof that the rotational losses of the rotation powered pulsar are not due to magnetodipole radiation but instead they are due to magnetic breaking of a relativistic wind ejected by the pulsars. In this regard we discuss the direct physical consequences from this conclusion for the pulsar physics.