  To better model the efficient production of cosmic rays (CRs) in supernova
remnants (SNRs) with the associated coupling between CR production and SNR
dynamics, we have generalized an existing cr-hydro-NEI code (i.e., Ellison et
al. 2012) to include the following processes: (1) an explicit calculation of
the upstream precursor structure including the position dependent flow speed,
density, temperature, and magnetic field strength; (2) a momentum and space
dependent CR diffusion coefficient; (3) an explicit calculation of magnetic
field amplification (MFA); (4) calculation of the maximum CR momentum using the
amplified magnetic field; (5) a finite Alfven speed for the particle scattering
centers; and (6) the ability to accelerate a superthermal seed population of
CRs as well as the ambient thermal plasma. While a great deal of work has been
done modeling SNRs, most work has concentrated on either the continuum emission
from relativistic electrons or ions, or the thermal emission from the shock
heated plasma. Our generalized code combines these elements and describes the
interplay between CR production and SNR evolution, including the nonlinear
coupling of efficient diffusive shock acceleration (DSA), based mainly on the
work of P. Blasi and co-workers, and a non-equilibrium ionization (NEI)
calculation of thermal X-ray line emission. We believe our generalized model
will provide a consistent modeling platform for SNRs, including those
interacting with molecular clouds, and improve the interpretation of current
and future observations, including the high-quality spectra expected from
Astro-H. SNR RX J1713.7-3946 is modeled as an example.
