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The gamma-ray emission of RX J1713.7-3946, despite being extensively studiedin the GeV and TeV domain, remains poorly understood. This is mostly because inthis range, two competing mechanisms can efficiently produce gamma rays: theinverse Compton scattering of accelerated electrons, and interactions ofaccelerated protons with nuclei of the ISM. In addition to the acceleration ofparticles from the thermal pool, the reacceleration of pre-existing CRs isoften overlooked, and shall in fact also been taken into account. Especially,because of the distance to the SNR ($\sim 1$ kpc), and the low density in whichthe shock is currently expanding ($\sim 10^{-2}$ cm$^{-3}$), there-acceleration of CR electrons pre-existing in the ISM, can account for asignificant fraction of the observed gamma-ray emission, and contribute to theshaping of the spectrum in the GeV-TeV range. Remarkably, this emission ofleptonic origin is found to be close to the level of the gamma-ray signal inthe TeV range, provided that the spectrum of pre-exisiting cosmic ray electronsis similar to the one observed in the local interstellar medium. The overallgamma-ray spectrum of RX J1713.7-3946 is naturally produced as the sum of aleptonic emission from reaccelerated CR electrons, and a subdominant hadronicemission from accelerated protons. We also argue that neutrino observationswith next-generation detectors might lead to a detection even in the case of alepto-hadronic origin of the gamma-ray emission.

Gamma rays and neutrinos from RX J1713.7-3946 in a lepto-hadronic scenario