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Observational Signatures of Particle Acceleration in Supernova Remnants

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Abstract

We evaluate the current status of supernova remnants as the sources of Galactic cosmic rays. We summarize observations of supernova remnants, covering the whole electromagnetic spectrum and describe what these observations tell us about the acceleration processes by high Mach number shock fronts. We discuss the shock modification by cosmic rays, the shape and maximum energy of the cosmic-ray spectrum and the total energy budget of cosmic rays in and surrounding supernova remnants. Additionally, we discuss problems with supernova remnants as main sources of Galactic cosmic rays, as well as alternative sources.

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Notes

  1. Note that this is the velocity relevant for the physical conditions behind the shock front (outside of the reverse shock).

  2. The upstream region is the region in front of the shock, i.e. outside the remnant for the forward shock.

  3. Note that the power-law index of a radio spectrum (α) is defined for a flux energy density, whereas in X-rays one use the spectral index (Γ) for the number density flux, the relation between the two indices is Γ=α+1. If the number density of the electron distribution is labeled q, we have that q=2α+1=2Γ−1.

  4. Note that some regions were excluded from the fit, for example for Tycho (West) only the emission between 237′′ and 255′′ was fitted, as the emission closer to the center may also have a thermal bremsstrahlung origin.

  5. There has been little attention to this issue, but see http://online.itp.ucsb.edu/online/astroplasmas_c09/vink/pdf/Vink_AstroPlasmasConf_KITP.pdf.

  6. Note that Katsuda et al. (2010b) uses a similar formalism, but with slightly different dependencies as they also consider the change in the amplified magnetic field.

  7. Sometimes the effect of multiplicity and cross section is combined in an inclusive cross section \(\sigma(E_{\mathrm{p,incl}})\) (e.g. Dermer 1986; Kamae et al. 2006).

  8. For example, for the Sedov solution in a uniform medium, R∝t 2/5 we have F=4πn H(R)R 2 v∝t 1/5. Whereas for the Sedov solution inside a stellar wind, R∝t 2/3, we get F=4πn H(R)R 2 v∝v∝t −1/3.

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Acknowledgements

We thank the anonymous referee for carefully reading the manuscript. The authors thank the ISSI in Bern for their hospitality and for organizing the workshop that resulted in this chapter. This work has been supported by SAO grant GO0-11072X (E.A.H.). A.M.B. was supported in part by the Russian government grant 11.G34.31.0001 to Sankt-Petersburg State Politechnical University, and also by the RAS Presidium Program and by the RFBR grant 11-02-12082. He performed the simulations at the Joint Supercomputing Center (JSCC RAS) and the Supercomputing Center at Ioffe Institute, St. Petersburg.

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Authors and Affiliations

  1. Department of Astronomy and Astrophysics, 525 Davey Laboratory, The Pennsylvania State University, University Park, PA, 16802, USA

    E. A. Helder

  2. Astronomical Institute Anton Pannekoek, Universiteit van Amsterdam, Postbus 94249, 1090 GE, Amsterdam, The Netherlands

    J. Vink

  3. Ioffe Institute for Physics and Technology, St. Petersburg State Politechnical University, 194021, St. Petersburg, Russia

    A. M. Bykov

  4. Theory Center, Institute of Particle and Nuclear Studies, KEK (High Energy Accelerator Research Organization), 1-1 Oho, Tsukuba, 305-0801, Japan

    Y. Ohira

  5. Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA, 02138, USA

    J. C. Raymond

  6. Astroparticule et Cosmologie, Universitè Paris7/CNRS/CEA, Batiment Condorcet, 75013, Paris, France

    R. Terrier

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Helder, E.A., Vink, J., Bykov, A.M. et al. Observational Signatures of Particle Acceleration in Supernova Remnants. Space Sci Rev 173, 369–431 (2012). https://doi.org/10.1007/s11214-012-9919-8

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