High-energy cosmic-ray electrons in the Galaxy

Research output: Contribution to journalArticle

5 Citations (Scopus)

Abstract

The intensity of cosmic-ray electrons is only ∼1% of the protons at 10 GeV, and decreases very rapidly with energy to be ∼0.1% of protons at 1 TeV. Nevertheless, electrons in cosmic-rays have unique features, complementary to all other cosmic-ray nucleonic components, because they enable us to find the origins of cosmic-rays and the properties of their propagation mechanisms in the Galaxy. High-energy electrons lose energy by synchrotron and inverse Compton processes during the propagation in the Galaxy. Since the energy loss rate by these processes is proportional to the square of energy, TeV electrons accelerated in the sources at distances larger than ∼1 kpc, or ages greater than a few 105 yr, cannot reach the solar system. This suggests that some nearby sources leave unique signatures in the form of identifiable structures in the energy spectrum of TeV electrons, and show increases of the flux towards the sources. In this paper, I review the past observations of high-energy cosmic-ray electrons and discuss their astrophysical significance.

Original languageEnglish
Pages (from-to)477-485
Number of pages9
JournalAdvances in Space Research
Volume42
Issue number3
DOIs
Publication statusPublished - 2008 Aug 5

Fingerprint

Galaxies
Cosmic rays
cosmic ray
cosmic rays
galaxies
electron
Electrons
energy
electrons
Protons
nucleonics
protons
propagation
solar system
Solar system
high energy electrons
Synchrotrons
astrophysics
synchrotrons
energy spectra

Keywords

  • Cosmic-ray electrons
  • Cosmic-ray origin
  • Supernova remnants

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

High-energy cosmic-ray electrons in the Galaxy. / Yoshida, Kenji.

In: Advances in Space Research, Vol. 42, No. 3, 05.08.2008, p. 477-485.

Research output: Contribution to journalArticle

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