Simulated synchrotron and Inverse Compton emission from Pulsar Wind Nebulae
Delia Volpi (1), Luca Del Zanna (1), Elena Amato (2), Niccolo, Bucciantini (3)((1) Univ. of Florence Italy, (2) Observatory of Arcetri, Italy, (3) Univ. of California at Berkeley)
TL;DR
This paper develops diagnostic tools for simulating and analyzing non-thermal emission maps of Pulsar Wind Nebulae, including synchrotron and inverse Compton processes, to compare with observational data.
Contribution
It introduces a comprehensive set of tools for synthetic emission mapping and applies them to Pulsar Wind Nebulae using relativistic MHD simulations.
Findings
Successfully reproduces synthetic emission maps
Provides insights into PWN emission mechanisms
Enhances comparison between models and observations
Abstract
We present a complete set of diagnostic tools aimed at reproducing synthetic non-thermal (synchrotron and/or Inverse Compton, IC) emissivity, integrated flux energy, polarization and spectral index simulated maps in comparison to observations. The time dependent relativistic magnetohydrodynamic (RMHD) equations are solved with a shock capturing code together with the evolution of the maximum particles energy. Applications to Pulsar Wind Nebulae (PWNe) are shown.
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