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A number of supernova remnants (SNRs) show nonthermal X-rays assumed to besynchrotron emission from shock accelerated TeV electrons. The existence ofthese TeV electrons strongly suggests that the shocks in SNRs are sources ofgalactic cosmic rays (CRs). In addition, there is convincing evidence frombroad-band studies of individual SNRs and elsewhere that the particleacceleration process in SNRs can be efficient and nonlinear. If SNR shocks areefficient particle accelerators, the production of CRs impacts the thermalproperties of the shock heated, X-ray emitting gas and the SNR evolution. Wereport on a technique that couples nonlinear diffusive shock acceleration,including the backreaction of the accelerated particles on the structure of theforward and reverse shocks, with a hydrodynamic simulation of SNR evolution.Compared to models which ignore CRs, the most important hydrodynamical effectsof placing a significant fraction of shock energy into CRs are larger shockcompression ratios and lower temperatures in the shocked gas. We compare ourresults, which use an approximate description of the acceleration process, witha more complete model where the full CR transport equations are solved (i.e.,Berezhko et al., 2002), and find excellent agreement for the CR spectrum summedover the SNR lifetime and the evolving shock compression ratio. The importanceof the coupling between particle acceleration and SNR dynamics for theinterpretation of broad-band continuum and thermal X-ray observations isdiscussed.Comment: Accepted for publication in A & A; 14 pages including 11 figure

Hydrodynamic simulation of supernova remnants including efficient particle acceleration