  We present a spherically symmetric, core-collapse model of SNR RX
J1713.7-3946 that includes a hydrodynamic simulation of the remnant evolution
coupled to the efficient production of cosmic rays (CRs) by nonlinear diffusive
shock acceleration (DSA). High-energy CRs that escape from the forward shock
(FS) are propagated in surrounding dense material that simulates either a
swept-up, pre-supernova shell or a nearby molecular cloud. The continuum
emission from trapped and escaping CRs, along with the thermal X-ray emission
from the shocked heated ISM behind the FS, integrated over the remnant, is
compared against broadband observations. Our results show conclusively that,
overall, the GeV-TeV emission is dominated by inverse-Compton from CR electrons
if the supernova is isolated regardless of its type, i.e., not interacting with
a >>100 Msun shell or cloud. If the SNR is interacting with a much larger mass
>10^4 Msun, pion-decay from the escaping CRs may dominate the TeV emission,
although a precise fit at high energy will depend on the still uncertain
details of how the highest energy CRs are accelerated by, and escape from, the
FS. Based on morphological and other constraints, we consider the 10^4 Msun
pion-decay scenario highly unlikely for SNR RX J1713.7-3946 regardless of the
details of CR escape. Importantly, even though CR electrons dominate the
GeV-TeV emission, the efficient production of CR ions is an essential part of
our leptonic model.
