Spectral features in the cosmic ray fluxes

Abstract

The cosmic ray energy distributions contain spectral features, that is narrow energy regions where the slope of the spectrum changes rapidly. The identification and study of these features is of great importance to understand the astrophysical mechanisms of acceleration and propagation that form the spectra. In first approximation a spectral feature in often described as a discontinuous change in slope, however very valuable information is also contained in its width, that is the length of the interval in logarithm of energy where the change in spectral index develops. In this work we discuss the best way to define and parametrize the width a spectral feature, and for illustration discuss some of the most prominent known structures.

arXiv comment15 pages, 9 figures

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Cited by in corpus (12)

• Measurement of the cosmic-ray energy spectrum above $2.5\times 10^{18}$ eV using the Pierre Auger Observatory
• Measurement of the cosmic ray helium energy spectrum from 70 GeV to 80 TeV with the DAMPE space mission
• Features of the energy spectrum of cosmic rays above $2.5\times 10^{18}$ eV using the Pierre Auger Observatory
• Diffuse Galactic gamma ray flux at very high energy
• Cosmic ray production in supernovae
• The shape of the cosmic ray proton spectrum
• Dynamical Effects of Cosmic Rays on the Medium Surrounding Their Sources
• Cosmic-ray generated bubbles around their sources
• The spectral shapes of the fluxes of electrons and positrons and the average residence time of cosmic rays in the Galaxy
• Atmospheric Neutrinos
• Galactic Gamma-Ray Diffuse Emission at TeV energies with HAWC Data
• Detection of Cosmic Rays from ground: an Introduction