Astronomy and Astrophysics – Astrophysics – High Energy Astrophysical Phenomena
Scientific paper
2010-09-06
Astrophys.J.729:93,2011
Astronomy and Astrophysics
Astrophysics
High Energy Astrophysical Phenomena
8 pages, 5 figures, accepted for publication in ApJ
Scientific paper
10.1088/0004-637X/729/2/93
One of the most essential but uncertain processes for producing cosmic-rays (CRs) and their spectra is how accelerated particles escape into the interstellar space. We propose that the CR electron spectra at >~TeV energy can provide a direct probe of the CR escape complementary to the CR nuclei and gamma-rays. We calculate the electron spectra from a young pulsar embedded in the supernova remnant (SNR), like Vela, taking into account the energy-dependent CR escape. SNRs would accelerate and hence confine particles with energy up to 10^{15.5}eV. Only energetic particles can escape first, while the lower energy particles are confined and released later. Then the observed electron spectrum should have a low energy cutoff whose position marks the age of the pulsar/SNR. The low energy cutoff is observable in the $\gtrsim {\rm TeV}$ energy window, where other contaminating sources are expected to be few due to the fast cooling of electrons. The spectrum looks similar to a dark matter annihilation line if the low energy cutoff is close to the high energy intrinsic or cooling break. The future experiments such as CALET and CTA are capable of directly detecting the CR escape features toward revealing the origin of CRs.
Ioka Kunihito
Kashiyama Kazumi
Kawanaka Norita
Ohira Yutaka
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