The discussion will be focussed on stars expected to support oscillations whose physics is potentially sufficiently well understood for reasonably reliable seismological inferences to be anticipated.

This agenda is intended to stimulate thought and to promote further suggestions that are of interest or potential interest to the meeting. Please send us your suggestions ( by e-mail to mcunha@astro.up.pt), or talk to us during the first day of the meeting.

Part 1: synopsis

• Identify aspects of the internal structure that one may realistically hope to infer from seismic data (in connection to stellar type).
• Identify the different inference techniques and their limitations.
• Identify the data required to apply a given technique (e.g., number of individual frequencies, range of degrees, quality of the data, ...).

Part 2: Discussion

• Basic structure of stellar cores, by inversion or by calibrating seismic signatures: Can we determine the extent of convective cores, and the amount and distribution of the products of nuclear transmutation to use as indicators of age and of the nature of overshooting and double-diffusive convection (semiconvection)?
• Extent and structure of stellar convective envelopes: Can we calibrate the upper boundary layer and hope to learn about convective energy and momentum transport? Can we calibrate the signature of helium ionization and determine the helium abundance in stars?
• Is it possible to detect and calibrate a tachocline?
• To what extent can other aspects of the structure of stars be determined from low-degree data?
• Seismic evidence for accretion, mass loss.
• Incorporating non-seismic data into inferential procedures: e.g. cluster calibrations.