Schematic structure for the Crab Nebula. The pulsar wind--pulsar wind termination shock (MHD shock) is the same as that of the standard PWNe model (Kennel & Coroniti 1984), with the region around the pulsar being the pulsar wind, terminated at the MHD shock. Beyond the MHD shock is the nebula region, where the magnetic field is transported to the outer part. In contrast to the PWNe model, the nebula region is a mixture of the pulsar wind and SN ejecta, as the pulsar wind penetrates the ejecta and breaks out to its outer edge, leading the expansion of the nebula. At the outer edge of r_d = 2 pc, a detonation wave forms as the nebula expands into the ISM, converting the magnetic field energy in the nebula to thermal and radiative energy through MR within the detonation. Inside but close to the expansion detonation is the reverse shock, which amplifies the nebula magnetic field and transports it to the downstream of the expansion detonation.