Hostname: page-component-8448b6f56d-wq2xx Total loading time: 0 Render date: 2024-04-19T11:26:08.800Z Has data issue: false hasContentIssue false
  • English
  • Français

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
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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

References

Aharonian, F., Akhperjanian, A. G., Bazer-Bachi, A. R., et al. 2006a, Nature, 439, 695CrossRefGoogle Scholar
Aharonian, F., Akhperjanian, A. G., Bazer-Bachi, A. R., et al. 2006b, A&A, 449, 223Google Scholar
Aharonian, F., Akhperjanian, A. G., Bazer-Bachi, A. R., et al. 2006c, ApJ, 636, 777CrossRefGoogle Scholar
Aharonian, F., Akhperjanian, A. G., Bazer-Bachi, A. R., et al. 2006d, A&A (Letters), 448, L43Google Scholar
Aharonian, F., Akhperjanian, A. G., Bazer-Bachi, A. R., et al. 2007, A&A, 661, 236Google Scholar
Decourchelle, A., Ellison, D. C., & Ballet, J. 2000, ApJ (Letters), 543, L57CrossRefGoogle Scholar
Parizot, E., Marcowith, A., Ballet, J., & Gallant, Y. A. 2006, A&A, 453, 387Google Scholar
Porter, T. A., Moskalenko, I. V., & Strong, A. W. 2006, ApJ (Letters), 648, L29CrossRefGoogle Scholar
Warren, J. S., Hughes, J. P, Badenes, C., Ghavamian, P., McKee, C. F., Moffett, D., Plucinsky, P. P., Rakowski, C., Reynoso, E., & Slane, P. 2005, ApJ, 634, 376CrossRefGoogle Scholar