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Explicitly time-dependent, nonlinear kinetic theory of cosmic ray (CR)acceleration in supernova remnants (SNRs) has been employed to investigate theproperties of SNR RX J1713.7-3946. Observations of the nonthermal radio andX-ray emission spectra as well as earlier H.E.S.S. measurements of the veryhigh energy $\gamma$-ray emission were used to constrain the astronomical andthe particle acceleration parameters of the system. The model assumes that theobject was a core collapse supernova (SN) with a massive progenitor, has an ageof $\approx 1600$ yr and is at a distance of $\approx 1$ kpc. It is shown thatan efficient production of nuclear CRs, leading to strong shock modificationand a large downstream magnetic field strength $B_{\mathrm{d}}\sim100$ $\mu$G,can reproduce the observed synchrotron emission from radio to X-ray frequenciestogether with the \gr spectral characteristics as observed by the H.E.S.S.telescopes. Small-scale filamentary structures observed in nonthermal X-raysprovide empirical confirmation for this field amplification scenario whichleads to a strong depression of the inverse Compton and Bremsstrahlung fluxes.The results are compared with the latest H.E.S.S. observations.

Comparing a model of cosmic ray production in the supernova remnant RX J1713.7-3946 with observations