2009/03/26 by Giovanni Morlino, G. Morlino, Pasquale Blasi +3
Physics and Astronomy · #Acceleration #Astronomy #Astrophysics #Astrophysics and Cosmic Phenomena #Cosmic ray #Gamma ray #Gamma-ray bursts and supernovae #Hadron #Neutrino #Neutrino Physics Research #Neutrino detector #Neutrino oscillation #Nuclear physics #Particle acceleration #Photon #Physics #Supernova #Supernova remnant #Telescope #Ultra-high-energy cosmic ray #astro-ph.HE
paper · pdf · doi:10.1016/j.astropartphys.2009.03.007
published as Astropart.Phys.31:376-382,2009 · 11 pages, 3 figures, accepted for publication in Astropaticle Physics
arxiv created 2009/03/26 · openalex publication_date 2009/04/06 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
The supernova paradigm for the origin of galactic cosmic rays can be tested using multifrequency observations of both non-thermal and thermal emission from supernova remnants. The smoking gun of hadronic acceleration in these sources can, however, only be provided by the detection of a high energy neutrino signal. Here we apply the theory of non-linear particle acceleration at supernova shocks to the case of the supernova remnant RX J1713.7-3946, which is becoming the stereotypical example of a possible hadronic accelerator after the detection of high energy gamma rays by the HESS telescope. Our aim is twofold: on one hand we want to address the uncertainties in the discrimination between a hadronic and a leptonic interpretation of the gamma ray emission, mainly related to the possibility of a statistical uncertainty in the energy determination of the gamma ray photons in the TeV region. On the other we want to stress how a km cube neutrino telescope would break the degeneracy and provide evidence for efficient cosmic ray acceleration in RX J1713.7-3946. A 3 sigma evidence would require about two years of observation.