Escape of cosmic-ray electrons from supernova remnants

Details Escape of cosmic-ray electrons from supernova remnants Escape of cosmic-ray electrons from supernova remnants

2011-06-09

arxiv.org/abs/1106.1810v1

Astronomy and Astrophysics

Astrophysics

High Energy Astrophysical Phenomena

10 pages, 8 figures and 1 table, submitted to ApJ

Scientific paper

We investigate the escape of cosmic ray (CR) electrons from a supernova remnant (SNR) to the interstellar space. We show that CR electrons escape in order from high to low energy with a similar spectrum to CR nuclei, while the escape starts later than the beginning of the Sedov phase at an SNR age of 1-7 10^3 yrs and the maximum energy of runaway CR electrons is below the knee about 0.3-50 TeV because unlike CR nuclei, CR electrons lose their energy due to synchrotron radiation. Highest energy CR electrons will be directly probed by AMS-02, CALET, CTA and LHAASO experiments, or have been already detected by H.E.S.S. as the spectral cutoff. Furthermore, we also calculate the spatial distribution of runaway CR electrons and their radiation spectra around SNRs. Contrary to common belief, maximum-energy photons of synchrotron radiation around 1 keV are emitted by runaway CR electrons inside the SNR. Inverse Compton scattering by runaway CR electrons can dominate the gamma-ray emission from runaway CR nuclei via pion decay, and both are detectable by CTA and LHAASO as clues to the CR origin and the amplification of magnetic fluctuations around the SNR. We also discuss middle-aged and/or old SNRs as unidentified very-high-energy gamma-ray sources.

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