The most likely sources of high-energy cosmic-ray electrons in supernova remnants

T. Kobayashi, Y. Komori, K. Yoshida, J. Nishimura

研究成果: Article

219 引用 (Scopus)

抄録

Evidence of nonthermal X-ray emission and TeV gamma rays from supernova remnants (SNRs) have strengthened the hypothesis that primary Galactic cosmic-ray electrons are accelerated in SNRs. High-energy electrons lose energy via synchrotron and inverse Compton processes during propagation in the Galaxy. Because of these radiative losses, TeV electrons liberated from SNRs at distances larger than ∼1 kpc, or times older than ∼105 yr, cannot reach the solar system. We investigated the cosmic-ray electron spectrum observed in the solar system using an analytical method and considered several candidate sources among nearby SNRs that may contribute to the high-energy electron flux. In particular, we discuss the effects for the release time from SNRs after the explosion, as well as the deviation of a source spectrum from a simple power law. From this calculation, we found that some nearby sources, such as Vela, Cygnus Loop, or Monogem, could leave unique signatures in the form of identifiable structure in the energy spectrum of TeV electrons and show anisotropies toward the sources, depending on when the electrons were liberated from the remnant. This suggests that, in addition to providing information on the mechanisms of acceleration and propagation of cosmic rays, specific cosmic-ray sources can be identified through the precise electron observation in the TeV region.

元の言語English
ページ(範囲)340-351
ページ数12
ジャーナルAstrophysical Journal
601
発行部数1 I
DOI
出版物ステータスPublished - 2004 1 20
外部発表Yes

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supernova remnants
cosmic ray
cosmic rays
electron
energy
electrons
solar system
high energy electrons
primary cosmic rays
electron flux
propagation
explosions
synchrotrons
energy spectra
signatures
gamma rays
galaxies
deviation
explosion
analytical method

ASJC Scopus subject areas

  • Space and Planetary Science

これを引用

The most likely sources of high-energy cosmic-ray electrons in supernova remnants. / Kobayashi, T.; Komori, Y.; Yoshida, K.; Nishimura, J.

:: Astrophysical Journal, 巻 601, 番号 1 I, 20.01.2004, p. 340-351.

研究成果: Article

Kobayashi, T. ; Komori, Y. ; Yoshida, K. ; Nishimura, J. / The most likely sources of high-energy cosmic-ray electrons in supernova remnants. :: Astrophysical Journal. 2004 ; 巻 601, 番号 1 I. pp. 340-351.
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AU - Yoshida, K.

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AB - Evidence of nonthermal X-ray emission and TeV gamma rays from supernova remnants (SNRs) have strengthened the hypothesis that primary Galactic cosmic-ray electrons are accelerated in SNRs. High-energy electrons lose energy via synchrotron and inverse Compton processes during propagation in the Galaxy. Because of these radiative losses, TeV electrons liberated from SNRs at distances larger than ∼1 kpc, or times older than ∼105 yr, cannot reach the solar system. We investigated the cosmic-ray electron spectrum observed in the solar system using an analytical method and considered several candidate sources among nearby SNRs that may contribute to the high-energy electron flux. In particular, we discuss the effects for the release time from SNRs after the explosion, as well as the deviation of a source spectrum from a simple power law. From this calculation, we found that some nearby sources, such as Vela, Cygnus Loop, or Monogem, could leave unique signatures in the form of identifiable structure in the energy spectrum of TeV electrons and show anisotropies toward the sources, depending on when the electrons were liberated from the remnant. This suggests that, in addition to providing information on the mechanisms of acceleration and propagation of cosmic rays, specific cosmic-ray sources can be identified through the precise electron observation in the TeV region.

KW - Acceleration of particles

KW - Cosmic rays

KW - Gamma rays: theory

KW - Supernova remnants

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