HAL : in2p3-00369625, version 1

Code Bibliographique ADS : 2008AIPC.1085..308M

DOI : 10.1063/1.3076667

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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

(12/2008)

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 - AstroParticule et Cosmologie
2 :	Istituto di Astrofisica Spaziale e Fisica cosmica - INAF
3 :	SEDI - Service d'Electronique, des Détecteurs et d'Informatique

équipe(s) de recherche : APC - AHE

Thème(s)

:

Physique/Astrophysique/Phénomènes cosmiques de haute energie Planète et Univers/Astrophysique/Phénomènes cosmiques de haute energie

Mot(s)-clé(s) : pulsars – nebulae – gamma-ray spectra – X-ray spectra

in2p3-00369625, version 1

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Contributeur : Simone Lantz <>

Soumis le : Vendredi 20 Mars 2009, 15:07:18

Dernière modification le : Samedi 23 Juin 2012, 13:55:36