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4th International Meeting on High Energy Gamma-Ray Astronomy, Heidelberg : Allemagne (2008)
High-energy flux evolution of Pulsar Wind Nebulae
F. Mattana1, 2, M. Falanga3, D. Götz3, R. Terrier1, P. Esposito2, A. Pellizzoni, A. De Luca2, V. Marandon1, A. Goldwurm1, P. Caraveo2

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.
1 :  APC - UMR 7164 - AstroParticule et Cosmologie
2 :  Istituto di Astrofisica Spaziale e Fisica cosmica - INAF
3 :  SEDI - Service d'Electronique, des Détecteurs et d'Informatique
Physique/Astrophysique/Phénomènes cosmiques de haute energie

Planète et Univers/Astrophysique/Phénomènes cosmiques de haute energie
pulsars – nebulae – gamma-ray spectra – X-ray spectra