%0 Conference Proceedings
%T VHE,gamma-ray emitting pulsar wind nebulae discovered by HESS
%+ Laboratoire de Physique Théorique et Astroparticules (LPTA)
%A Gallant, Yves
%A Carrigan, S.
%A Djannati-Atai, A.
%A Funk, S.
%A Hinton, J. A.
%A Hoppe, S.
%A de Jager, O. C.
%A Khelifi, B.
%A Komin, Nukri
%A Kosack, K.
%A Lemiere, A.
%A Masterson, C.
%< avec comité de lecture
%Z LPTA:07-094
%( 40 YEARS OF PULSARS: MILLISECOND PULSARS, MAGNETARS AND MORE
%B AIP Conference: 40 Years of Pulsars
%C Montreal, Canada
%I AMER INST PHYSICS, 2 HUNTINGTON QUADRANGLE, STE 1NO1 D, MELVILLE, NY 11747-4501 USA
%V 983
%P 195-199
%8 2007-08-12
%D 2007
%K gamma-ray observations
%K pulsars
%K nebulae
%K ENERGY GAMMA-RAYS
%K XMM-NEWTON OBSERVATIONS
%K SUPERNOVA REMNANT
%K J1813-178
%K EMISSION
%K REVEAL
%Z Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO]
%Z Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO]Conference papers
%X Recent advances in very-high-energy (VHE) gamma-ray astronomy have opened a new observational window on the physics of pulsars. The high sensitivity of current imaging atmospheric Cherenkov telescopes, and in particular of the H.E.S.S. array, has already led to the discovery of about a dozen VHE-emitting pulsar wind nebulae (PWN) and PWN candidates. These include the plerions in the composite supernova remnants MSH 15-52, G 21.5-0.9, Kes 75, and Vela, two sources in the Kookaburra, and the nebula of PSR B 1823-13. This VHE emission is generally interpreted as inverse Compton emission from the relativistic electrons and positrons accelerated by the pulsar and its wind; as such, it can yield a more direct spatial and spectral view of the accelerated particles than can be inferred from observations of their synchrotron emission. The VHE-emitting PWNe detected by the H.E.S.S. telescopes are reviewed and the implications for pulsar physics discussed.
%G English
%L hal-00491483
%U https://hal.science/hal-00491483
%~ IN2P3
%~ LPTA
%~ CNRS
%~ UNIV-MONTP2
%~ UNIV-MONTPELLIER
%~ UM1-UM2