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Based largely on energy budget considerations and the observed cosmic-ray(CR) ionic composition, supernova remnant (SNR) blast waves are the most likelysources of CR ions with energies at least up to the "knee" near 3 PeV. Shocksin young shell-type TeV-bright SNRs are surely producing TeV particles, but theemission could be dominated by ions producing neutral pion-decay emission orelectrons producing inverse-Compton gamma-rays. Unambiguously identifying theGeV-TeV emission process in a particular SNR will not only help pin down theorigin of CRs, it will add significantly to our understanding of the diffusiveshock acceleration (DSA) mechanism and improve our understanding of supernovaeand the impact SNRs have on the circumstellar medium. In this study, weinvestigate the Vela Jr. SNR, an example of TeV-bright non-thermal SNRs. Weperform hydrodynamic simulations coupled with non-linear DSA andnon-equilibrium ionization near the forward shock (FS) to confront currentlyavailable multi-wavelength data. We find, with an analysis similar to that usedearlier for SNR RX J1713.7-3946, that self-consistently modeling the thermalX-ray line emission with the non-thermal continuum in our one-dimensional modelstrongly constrains the fitting parameters, and this leads convincingly to aleptonic origin for the GeV-TeV emission for Vela Jr. This conclusion isfurther supported by applying additional constraints from observation,including the radial brightness profiles of the SNR shell in TeV gamma-rays,and the spatial variation of the X-ray synchrotron spectral index. We willdiscuss implications of our models on future observations by thenext-generation telescopes.

A CR-hydro-NEI Model of Multi-wavelength Emission from the Vela Jr. Supernova Remnant (SNR RX J0852.0-4622)