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High-energy flux evolution of Pulsar Wind Nebulae

Abstract : The very high energy γ-ray spectra of Pulsar Wind Nebulae are interpreted as due to inverse Compton scattering of ultrarelativistic electrons on the ambient photons, whereas their X-ray spectra are due to synchrotron emission. We investigate the relation between the γ- and X-ray emission and the pulsars' spin-down luminosity and characteristic age. We find that the γ-to X-ray flux ratio of the nebulae is inversely proportional to the spin-down luminosity (~Ė-1.9) and to the characteristic age (~τc2.2) of the parent pulsar. We interpret these results as due to the evolution of the electron energy distribution and the nebular dynamics, supporting the idea of so-called relic pulsar wind nebulae. These empirical relations provide a new tool to classify unidentified diffuse γ-ray sources and to estimate the spin-down luminosity and characteristic age for four rotation powered pulsars with no detected pulsation from the X- and γ-ray properties of the associated pulsar wind nebulae.
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Contributor : Simone Lantz <>
Submitted on : Friday, March 20, 2009 - 3:07:18 PM
Last modification on : Friday, October 30, 2020 - 12:04:03 PM



F. Mattana, M. Falanga, D. Götz, R. Terrier, P. Esposito, et al.. High-energy flux evolution of Pulsar Wind Nebulae. 4th International Meeting on High Energy Gamma-Ray Astronomy, Jul 2008, Heidelberg, Germany. pp.308-311, ⟨10.1063/1.3076667⟩. ⟨in2p3-00369625⟩



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