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Fine Structure in Cosmic Ray Spectra

Fine Structure in Cosmic Ray Spectra. Tolya Erlykin and Arnold Wolfendale. Lebedev, Moscow. Durham University. The evolution of optical spectral structure. Continuum Indian Vedic Period 15 th Century Newton 18 th Century Fine structure Bunsen, Kirchoff 19 th Century

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Fine Structure in Cosmic Ray Spectra

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  1. Fine Structure in Cosmic Ray Spectra TolyaErlykin and Arnold Wolfendale Lebedev, Moscow Durham University

  2. The evolution of optical spectral structure Continuum Indian Vedic Period 15th Century Newton 18th Century Fine structure Bunsen, Kirchoff 19th Century Hyperfine Structure Michelson 1881 Red OrangeYellow Green Blue Violet Green Blue Orange

  3. The spectrum is smooth, apart from just two features, the knee and the ankle. • Not true! Log En I(E)

  4. If there are discrete sources (eg. Pulsars, SNR) there should be more structure, due to the stochastic nature of the sources, in space and time.

  5. Much evidence for SNR origin, starting with Bhat et al. (1985) for Loop I using SAS II diffuse gamma ray data. Results for E : 35-100 MeV (electrons mainly) and for E > 100 MeV (nuclei mainly). • Confirmation from later data, including HESS.

  6. Erlykin et al’s 2003 Monte Carlo Spectra for protons from random SNR and different propagation modes.

  7. (E)

  8. The knee The historic 1997 graph. Nowadays the ‘CNO’ peak is identified with Helium.

  9. The Monogem Ring SNR and pulsar Age 105 y X-Ray Image; 9o radius circle The ‘Local Source’(distance ~300 pc)

  10. The latest situation

  11. Probably the transition between Galactic and Extragalactic particles Wibig & W. The Ankle

  12. A new component? EW2012 Present in all nuclei, electrons and gamma rays. Local bubble? (PAMELA & ATIC) The Kink

  13. Rigidity of the Kink – And Sharpness

  14. Energy Spectra of Electrons in the ATIC Experiment

  15. FERMI-LAT GAMMAS

  16. The predicted TeV ‘bump’ A very tentative observation so far, from CREAM. A ΔlogIE3 bump of ≃ 0.15 near 10TeV, perhaps. We expect such bumps.

  17. CONCLUSIONS As time has gone on more and more structure has been seen, and this will continue. Strong clues as to cosmic ray origins will appear.

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