Energy spectra of abundant nuclei of primary cosmic rays from the data of ATIC-2 experiment: Final results
By A. Panov, J. Adams, H. Ahn, G. L. Bashinzhagyan, J. Watts, J. Wefel, J. Wu, O. Ganel, T. Guzik, V. Zatsepin and 10 more. 2009
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The final results of processing the data from the balloon-born experiment ATIC-2 (Antarctica, 2002–2003) for the energy spectra of protons and He, C, O, Ne, Mg, Si, and Fe nuclei, the spectrum of all particles, and the mean logarithm of atomic weight of primary cosmic rays as a function of energy are presented. The final results are based on improvement of the methods used earlier, in particular, considerably increased resolution of the charge spectrum. The preliminary conclusions on the significant difference in the spectra of protons and helium nuclei (the proton spectrum is steeper) and the non-power character of the spectra of protons and heavier nuclei (flattening of carbon spectrum at energies above 10 TeV) are confirmed. A complex structure of the energy dependence of the mean logarithm of atomic weight is found.
Subfields: Nuclear and High Energy Physics, Radiation
View Paper: https://www.semanticscholar.org/paper/98148b787297df06bd9cf7425870b0832a7c98c7
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In Nuclear and High Energy Physics
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- DISCREPANT HARDENING OBSERVED IN COSMIC-RAY ELEMENTAL SPECTRA (2010, methodology): “…fluxes are compared with selected previous data (Asakimori et al. 1998; Derbina et al. 2005; Zei et al. 2007; Ahn et al. 2007b; Alcaraz et al. 2000; Panov et al. 2009): CREAM-1 (filled circles), CREAM-2 (filled squares), AMS (stars), BESS (open squares), JACEE (X), RUNJOB (inverted triangles),…”