Volume 495, Number 1, February III 2009
|Page(s)||9 - 13|
|Published online||14 January 2009|
Gamma-ray spectrum of RX J1713.7-3946 in the Fermi era and future detection of neutrinos
Department of Physical Science, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526, Japan e-mail: firstname.lastname@example.org; email@example.com
2 Physics Department, Lancaster University, LA1 4YB, UK e-mail: firstname.lastname@example.org
Accepted: 5 December 2008
The recently launched satellite, Fermi Gamma-ray Space Telescope , is expected to find out if cosmic-ray (CR) protons are generated from supernova remnants (SNRs), especially RX J1713.7-3946, by observing the GeV-to-TeV γ-rays. The GeV emission is thought to be bright if the TeV emission is hadronic, i.e., of proton origin, while dim if leptonic. We reexamine the above view using a simple theoretical model of nonlinear acceleration of particles to calculate the gamma-ray spectrum of Galactic young SNRs. If the nonlinear effects of CR acceleration are considered, it may be impossible to distinguish the evidence of proton acceleration from leptonic in the γ-ray spectrum of Galactic young SNRs like RX J1713.7-3946. On the other hand, future km3-class neutrino observations will likely find a clear evidence of the proton acceleration there.
Key words: acceleration of particles / ISM: supernova remnants / gamma rays: theory
© ESO, 2009
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