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The evolution and spectral properties of stars on the AGB are significantlyaffected by mass loss through dusty stellar winds. Dynamic atmosphere and windmodels are an essential tool for studying these evolved stars, bothindividually and as members of stellar populations, to understand theircontribution to the integrated light and chemical evolution of galaxies.  This paper is part of a series testing state-of-the-art atmosphere and windmodels of carbon stars against observations, and making them available for usein various theoretical and observational studies.  We have computed low-resolution spectra and photometry (in the wavelengthrange 0.35-25 mu) for a grid of 540 dynamic models with stellar parameterstypical of solar-metallicity C-rich AGB stars and with a range of pulsationamplitudes. The models cover the dynamic atmosphere and dusty outflow (ifpresent), assuming spherical symmetry, and taking opacities of gas-phasespecies and dust grains consistently into account. To characterize thetime-dependent dynamic and photometric behaviour of the models in a concise waywe defined a number of classes for models with and without winds.  Comparisons with observed data in general show a quite good agreement forexample regarding mass-loss rates vs. (J-K) colours or K magnitudes vs. (J-K)colours. Some exceptions from the good overall agreement, however, are foundand attributed to the range of input parameters (e.g. relatively high carbonexcesses) or intrinsic model assumptions (e.g. small particle limit for grainopacities).  While current results indicate that some changes in model assumptions andparameter ranges should be made in the future to bring certain syntheticobservables into better agreement with observations, it seems unlikely thatthese pending improvements will significantly affect the mass-loss rates of themodels.

Synthetic photometry for carbon-rich giants. IV. An extensive grid of dynamic atmosphere and wind models