The present is a period of dramatic evolution of the study of stellar structure and evolution, in large part owing to the possibilities offered by the rapidly expanding **data** on stellar oscillations. The resulting frequencies are expected to provide stringent constraints on stellar properties, including the structure of stellar interiors, and hence challenge our understanding of stellar internal physics and stellar evolution. An obvious requirement for this is that observations are made of a sufficiently broad sample of stars, with sufficient sensitivity and of sufficient duration to secure the required frequency precision. Such observations are now resulting from the CoRoT and Kepler space missions (e.g., Baglin et al. 2006;Borucki et al. 2010), and further improvements are promised by dedicated ground-based facilities for radialvelocity observations (e.g., Grundahl et al. 2009). However, this is not all: we must also be able to analyse the basic observations to extract reliable frequencies, as well as to identify the observed modes. Also, stellar modelling must be sufficiently reliable and accurate that the assumptions about stellar internal physics are faithfully reflected in the frequencies computed from the resulting models. Although substantial progress is being made both in the **data** analysis and the modelling, it is probably fair to say that further efforts are required in these directions.