Klein-Nishina effect and the cosmic ray electron spectrum

Abstract

Radiative energy losses are very important in regulating the cosmic ray electron and/or positron (CRE) spectrum during their propagation in the Milky Way. Particularly, the Klein-Nishina (KN) effect of the inverse Compton scattering (ICS) results in less efficient energy losses of high-energy electrons, which is expected to leave imprints on the propagated electron spectrum. It has been proposed that the hardening of CRE spectra around 50 GeV observed by Fermi-LAT, AMS-02, and DAMPE could be due to the KN effect. We show in this work that the transition from the Thomson regime to the KN regime of the ICS is actually quite smooth compared with the approximate treatment adopted in some previous works. As a result, the observed spectral hardening of CREs cannot be explained by the KN effect. It means that an additional hardening of the primary electrons spectrum is needed. We also provide a parameterized form for the accurate calculation of the ICS energy-loss rate in a wide energy range.

arXiv comment5 pages, 3 figures, 1 table, author-edited version

References in corpus (24)

• Observation of an anomalous positron abundance in the cosmic radiation
• The Temperature of the Cosmic Microwave Background
• Propagation of cosmic-ray nucleons in the Galaxy
• Measurement of the Cosmic Ray e+ plus e- spectrum from 20 GeV to 1 TeV with the Fermi Large Area Telescope
• The energy spectrum of cosmic-ray electrons at TeV energies
• Direct detection of a break in the teraelectronvolt cosmic-ray spectrum of electrons and positrons
• The cosmic-ray electron flux measured by the PAMELA experiment between 1 and 625 GeV
• The Most Likely Sources of High Energy Cosmic-Ray Electrons in Supernova Remnants
• Klein-Nishina Effects in the Spectra of Non-Thermal Sources Immersed in External Radiation Fields
• Cosmic-ray electron+positron spectrum from 7 GeV to 2 TeV with the Fermi Large Area Telescope
• Galactic electrons and positrons at the Earth:new estimate of the primary and secondary fluxes
• Dark Matter and Pulsar Origins of the Rising Cosmic Ray Positron Fraction in Light of New Data From AMS
• Interpretation of AMS-02 electrons and positrons data
• Energy Spectrum of Cosmic-ray Electron and Positron from 10 GeV to 3 TeV Observed with the Calorimetric Electron Telescope on the International Space Station
• Propagation of cosmic rays in the AMS-02 era
• Constraints on the distribution of supernova remnants with Galactocentric radius
• Quantitative study of the AMS-02 electron/positron spectra: implications for the pulsar and dark matter properties
• Klein-Nishina steps in the energy spectrum of galactic cosmic ray electrons
• On the Energy Spectra of GeV/TeV Cosmic Ray Leptons
• Reconcile the AMS-02 positron fraction and Fermi-LAT/HESS total $e^{\pm }$ spectra by the primary electron spectrum hardening
• Dark Matter Particle Explorer observations of high-energy cosmic ray electrons plus positrons and their physical implications
• Signature of Energy Losses on the Cosmic Ray Electron Spectrum
• Perspective on the cosmic-ray electron spectrum above TeV
• The `excess' of primary cosmic ray electrons

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• Where are the Pevatrons that Form the Knee in the Spectrum of the Cosmic Ray Nucleon Component around 4 PeV?
• The diffuse extragalactic gamma-ray background radiation: star-forming galaxies are not the dominant component
• Discrete treatment of inverse Compton scattering: implications on parameter estimation in gamma-ray astronomy
• PHECT: A lightweight computation tool for pulsar halo emission
• Mirage Sources and Large TeV Halo-Pulsar Offsets: Exploring the Parameter Space
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