A better understanding of the mechanisms that excite stellar oscillations and of the resulting and amplitudes and line profiles of such oscillations , is needed to design the observing programme, to aid in mode recognition, and to understand the underlying physical processes, especially of convection and turbulence. We will hear of some progress that has been made to date in the following presentations but much more needs to be done. The very important effects of moderate to rapid rotation, where mode coupling is important, needs particular attention as is emphasised in the sepaerate session of this meeting.

a. What are the expected amplitudes of low l p-modes on solar type stars?
Such modes are believed to be stochastically excited by convection. Is our understanding of both convection and of stochastic excitation reliable enough for us to estimate what amplitudes on other stars using scaling-law estimates? Does the power "observed" on the few candidates for ground based detection of p-mode oscillations support these estimates?

b. What is the expected decrease in amplitude with l value?
This depends on both the predicted amplitude as a function of l value and on the visibility effect - that is the averaging over the visible hemisphere. Are we confident that we are able to do either?

c. What do we expect to see on moderate amplitude pulsators, eg. delta Scutis?
Will we see a veritable "forest" of modes and be unable to identify them? Can we predicted the amplitudes as a function of l values and rotational splitting? Do we understand why some modes have larger amplitudes than others?

d. What is the effect of moderate to rapid rotation?
This is considered in a seperate session but we are still far from answering the question.

e. Understanding Convection?
If we are able to measure line shapes and amplitudes will we be able to use this to advance our understanding of the properties of the excitation mechanisms. In particular will we be able to advance our understanding of turbulent convection - going beyond the simple (indeed naive) mixing length models?

f. Opacity and equation of state
Will we be able to enhance our knowledge of the opacity and equation of state of stellar material from details of line profiles and amplitudes of modes excited by the kappa mechanism?

g. Mode amplitudes and mode interaction
Will we be able to understand what determines which modes have larger amplitudes and the physics of mode interaction. This is of course particularly important for rapidly rotating stars.

h. And more ...

There are many questions to be answered before we can with confidence predict what we are likely to see with COROT.

There are many more questions to be answered before we will be able, with confidence to interpret the observations of COROT in terms of mode recognition and the physics of excitation and amplitude determination.

A start towards answering some of these questions is made in the following papers by Samadi, Scuflaire, De Ridder, and Kupka.