abstract:
Pulsar wind Nebulae (PWNe) form as a result of the bulk of pulsar rotational energy loss via the emission of a relativistic wind of particles. The winds, being supersonic with respect to the interstellar medium, produce a termination shock where particles are accelerated and emit photons at all frequencies, from radio to TeV energies, via non-thermal processes such as synchrotron and inverse Compton. Reverberation is the period of PWN evolution when the reverse shock created by the supernova explosion travels back towards the pulsar, compressing the wind bubble. We study the evolution of this non-thermal radiation along the pulsar lifetime, especially the reverberation phase, analyzing the changes produced to the spectral energy distribution and find for a short time PWNe emit more in X-rays and other frequencies than what they have as rotational energy at the time due to the adiabatic heating from the environment. We also estimated via Monte Carlo simulations how many Galactic PWNe are expected to be reverberating or in a superefficiency stage at any given time.
