To better model the efficient production of cosmic rays (CRs) in supernovaremnants (SNRs) with the associated coupling between CR production and SNRdynamics, we have generalized an existing cr-hydro-NEI code (i.e., Ellison etal. 2012) to include the following processes: (1) an explicit calculation ofthe upstream precursor structure including the position dependent flow speed,density, temperature, and magnetic field strength; (2) a momentum and spacedependent CR diffusion coefficient; (3) an explicit calculation of magneticfield amplification (MFA); (4) calculation of the maximum CR momentum using theamplified magnetic field; (5) a finite Alfven speed for the particle scatteringcenters; and (6) the ability to accelerate a superthermal seed population ofCRs as well as the ambient thermal plasma. While a great deal of work has beendone modeling SNRs, most work has concentrated on either the continuum emissionfrom relativistic electrons or ions, or the thermal emission from the shockheated plasma. Our generalized code combines these elements and describes theinterplay between CR production and SNR evolution, including the nonlinearcoupling of efficient diffusive shock acceleration (DSA), based mainly on thework of P. Blasi and co-workers, and a non-equilibrium ionization (NEI)calculation of thermal X-ray line emission. We believe our generalized modelwill provide a consistent modeling platform for SNRs, including thoseinteracting with molecular clouds, and improve the interpretation of currentand future observations, including the high-quality spectra expected fromAstro-H. SNR RX J1713.7-3946 is modeled as an example.
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