We present a 3-dimensional model of supernova remnants (SNRs) where thehydrodynamical evolution of the remnant is modeled consistently with nonlineardiffusive shock acceleration occuring at the outer blast wave. The modelincludes particle escape and diffusion outside of the forward shock, andparticle interactions with arbitrary distributions of external ambientmaterial, such as molecular clouds. We include synchrotron emission andcooling, bremsstrahlung radiation, neutral pion production, inverse-Compton(IC), and Coulomb energy-loss. Boardband spectra have been calculated fortypical parameters including dense regions of gas external to a 1000 year oldSNR. In this paper, we describe the details of our model but do not attempt adetailed fit to any specific remnant. We also do not include magnetic fieldamplification (MFA), even though this effect may be important in some youngremnants. In this first presentation of the model we don't attempt a detailedfit to any specific remnant. Our aim is to develop a flexible platform, whichcan be generalized to include effects such as MFA, and which can be easilyadapted to various SNR environments, including Type Ia SNRs, which explode in aconstant density medium, and Type II SNRs, which explode in a pre-supernovawind. When applied to a specific SNR, our model will predict cosmic-ray spectraand multi-wavelength morphology in projected images for instruments withvarying spatial and spectral resolutions. We show examples of these spectra andimages and emphasize the importance of measurements in the hard X-ray, GeV, andTeV gamma-ray bands for investigating key ingredients in the accelerationmechanism, and for deducing whether or not TeV emission is produced by IC fromelectrons or neutral pions from protons.
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