  Aims. The hadronic vs. leptonic origin of the gamma-ray emission from the
Supernova Remnant RX J1713.7-3946 is discussed both in the light of new
observations and from a theoretical point of view.
  Methods. The existing good spatial correlation of the gamma-ray emission and
the nonthermal X-ray emission is analyzed theoretically. In addition, the
recently published new H.E.S.S. observations define the energy spectrum more
precisely, in particular at the high and low energy ends of the instrument's
dynamical range. There now exist much more constraining X-ray observations from
Suzaku that extend substantially beyond 10 keV. These new data are compared
with the authors' previous theoretical predictions, both for dominant hadronic
and for simple inverse Compton models.
  Results. Apart from the well-known MHD correlation between magnetic field
strength and plasma density variations, emphasized by the wind-bubble-structure
of the remnant, it is argued that the regions of magnetic field amplification
also are correlated with enhanced densities of accelerated nuclear particles
and the associated streaming instabilities. Therefore a correlation of
nonthermal X-ray and \gr emission is not only possible but even to be expected
for a hadronic emission scenario. A leptonic origin of the gamma-ray emission
would require an implausibly uniform strength of the magnetic field. The
observational and theoretical inferences about substantial field amplification
in this remnant agree very well with the recent X-ray and \gr observations.
  Conclusions. All this argues strongly for the dominance of hadronic \grs in
the \gr emission spectrum and a fortiori for an overwhelming contribution of
nuclear cosmic ray particles to the nonthermal energy in this remnant.
