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Galactic acceleration phenomena

Published online by Cambridge University Press:  01 August 2006

Yves A. Gallant
Yves A. Gallant*
Affiliation:
Laboratoire de Physique Théorique et Astroparticules, UMR 5027, CNRS/IN2P3, Université Montpellier II, 34095 Montpellier Cedex 5, France email: gallant@lpta.in2p3.fr
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Abstract

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I review the current status of our observational knowledge of prominent classes of particle accelerators in the Galaxy, namely shell-type supernova remnants (SNRs) and pulsar wind nebulae. I highlight in particular the contribution of the recent improvement in sensitivity of very-high-energy (VHE) γ-ray observations, which are currently the most direct probe of particle acceleration in the Galaxy up to energies of several hundreds of TeV.

Shell-type SNRs have long been proposed as sources of the Galactic cosmic rays. In recent years, X-ray observations have revealed very thin, non-thermal rims in many young SNRs, and I discuss the implications of these observations for magnetic field amplification and the maximum particle energy attainable by acceleration at the blast wave. I then review the current status of the evidence for accelerated nuclei in these objects, and summarise current uncertainties.

The most numerous class of identified Galactic VHE gamma-ray sources is currently that of pulsar wind nebulae (PWNe). The emission from these objects is generally assumed to be predominantly leptonic, and I outline the new information provided by VHE gamma-ray observations beyond what could be inferred from observations of synchrotron emission.

Keywords

acceleration of particlescosmic raysgamma rays: observationssupernova remnantsshock wavesmagnetic fieldspulsars: generalradiation mechanisms: nonthermal
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Highlights of Astronomy 14: Highlights of Astronomy , August 2006 , pp. 91 - 92
Copyright
Copyright © International Astronomical Union 2007

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