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Context. The large quantity of high-quality asteroseismic data that obtainedfrom space-based photometric missions and the accuracy of the resultingfrequencies motivate a careful consideration of the accuracy of computedoscillation frequencies of stellar models, when applied as diagnostics of themodel properties.  Aims. Based on models of red-giant stars that have been independentlycalculated using different stellar evolution codes, we investigate the extentto which the differences in the model calculation affect the model oscillationfrequencies.  Methods. For each of the models, which cover four different masses anddifferent evolution stages on the red-giant branch, we computed full sets oflow-degree oscillation frequencies using a single pulsation code and, fromthese frequencies, typical asteroseismic diagnostics. In addition, we carriedout preliminary analyses to relate differences in the oscillation properties tothe corresponding model differences.  Results. In general, the differences in asteroseismic properties between thedifferent models greatly exceed the observational precision of theseproperties, in particular for the nonradial modes whose mixed acoustic andgravity-wave character makes them sensitive to the structure of the deepstellar interior. In some cases, identifying these differences led toimprovements in the final models presented here and in Paper I; here weillustrate particular examples of this.  Conclusions. Further improvements in stellar modelling are required in orderfully to utilise the observational accuracy to probe intrinsic limitations inthe modelling. However, our analysis of the frequency differences and theirrelation to stellar internal properties provides a striking illustration of thepotential of the mixed modes of red-giant stars for the diagnostics of stellarinteriors.

The Aarhus red giants challenge II. Stellar oscillations in the red giant branch phase