Motivation

In the last two decades, we are witnessing enormous progress in observations of stellar oscillations. The precision of radial velocity measurements has reached the 1 cm/s level. The photometric precision is now at the 10^-4 mag level, for ground-based networks, or even better for space observations. Massive photometric surveys, such as MACHO, OGLE or ASAS, provided a wealth of data on various types of pulsating variables which has not yet been fully explored. Interpretation and exploitation of existing data in the context of stellar physics is very much lagging behind.

This is why, at the Wrocław Workshop, we want to put the emphasis on the difficult but fascinating road from observations to constraints on stellar parameters and physical processes in their interiors. Theory is involved in every step of this road, beginning with association frequency peaks with modes of stellar oscillations. A guidance from theory is always used to single out peaks corresponding to stellar eigenmodes in complicated oscillation spectra. In many cases, knowledge which modes may be exited in the star is a useful hint.

The main connection between asteroseismology and stellar evolution theory goes through construction of seismic models, which satisfy all observational and theoretical constraints. Such models yield information on element mixing, opacity, efficiency of convection and non-uniform rotation. However, even the very occurrence of pulsation teaches us something about evolutionary processes in outer layers, as best exemplified by sdB stars.

As always, at asteroseismic meeting, we foresee talks on current and future observational projects as well as on new results for all types of multiperiodic pulsators. However, the emphasis will be put on what we can learn about stars from their variability.