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 solving both advection and diffusion of non-thermal particles in a self-consistent way to satisfy the momentum and energy conservation laws. Assuming spherically symmetric (1--D) 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 photon index are well consistent with observations. Our model suggests that particles escaped from the nebula significantly contribute to the gamma-ray flux. A $\gamma$-ray halo larger than the radio nebula is predicted in our model.

12 pages, 13 figures, accepted for publication in ApJ

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• A Comprehensive Study of the Spectral Variation and the Brightness Profile of Young Pulsar Wind Nebulae
• Spectral Break of Energetic Pulsar Wind Nebulae Detected with Wideband X-ray Observations
• Pulsar Wind Nebulae
• SED modelling of broadband emission in the pulsar wind nebula 3C 58
• Spatio-spectral-temporal Modelling of Two Young Pulsar Wind Nebulae