Outflow and Emission Model of Pulsar Wind Nebulae with the Back Reaction of Particle Diffusion

Abstract

We present a new pulsar wind nebula (PWN) model that solves both advection and diffusion of nonthermal particles in a self-consistent way to satisfy the momentum and energy conservation laws. Assuming spherically symmetric (1D) steady outflow, we calculate the emission spectrum integrating over the entire nebula and the radial profile of the surface brightness. We find that the back reaction of the particle diffusion modifies the flow profile. The photon spectrum and the surface brightness profile are different from the model calculations without the back reaction of the particle diffusion. Our model is applied to the two well-studied PWNe, 3C 58 and G21.5-0.9. By fitting the spectra of these PWNe, we determine the parameter sets and calculate the radial profiles of X-ray surface brightness. For both the objects, obtained profiles of X-ray surface brightness and the photon index are well consistent with observations. Our model suggests that particles that have escaped from the nebula significantly contribute to the γ -ray flux. A γ -ray halo larger than the radio nebula is predicted in our model.