VHE,γ-ray emitting pulsar wind nebulae discovered by HESS

被引：0
|
作者：
Gallant, Y. A. [1 ]
Carrigan, S. [2 ]
Djannati-Atai, A. [3 ]
Funk, S. [4 ]
Hinton, J. A. [5 ]
Hoppe, S. [2 ]
de Jager, O. C. [6 ]
Khelifi, B. [7 ]
Komin, Nu. [1 ]
Kosack, K. [2 ,4 ]
Lemiere, A. [3 ]
Masterson, C.
机构：
[1] Univ Montpellier 2, CNRS, IN2P3, LPTA, Pl Eugene Bataillon, F-34095 Montpellier, France
[2] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany
[3] Univ Paris 07, CNRS, Astroparticule Cosmol, F-75025 Paris, France
[4] SLAC, Kavli Inst Astoparticle Phys & Cosmol, Menlo Pk, CA 94025 USA
[5] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England
[6] Northwestern Univ, Univ Space Phys, Potchefstroom SA-2520, South Africa
[7] Ecole Polytech, Lab Leprin Ringuet, F-91128 Palaiseau, France
[8] Dublin Inst Adv Studies, Dublin, Ireland
来源：
40 YEARS OF PULSARS: MILLISECOND PULSARS, MAGNETARS AND MORE | 2007年 / 983卷
基金：
英国科学技术设施理事会;
关键词：
gamma-ray observations; pulsars; nebulae;
D O I：
暂无
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
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.
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页码：195 / +
页数：2
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