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Helioseismology has been widely acclaimed as having been a great success: itappears to have answered nearly all the questions that we originally asked,some with unexpectedly high precision. We have learned how the sound speed andmatter density vary throughout almost all of the solar interior -- which not sovery long ago was generally considered to be impossible -- we have learned howthe Sun rotates, and we have a beautiful picture, on a coffee cup, of thethermal stratification of a sunspot, and also an indication of the materialflow around it. We have tried, with some success at times, to apply ourfindings to issues of broader relevance: the test of the General Theory ofRelativity via planetary orbit precession (now almost forgotten because theissue has convincingly been closed, albeit no doubt temporarily), the solarneutrino problem, the manner of the transport of energy from the centre to thesurface of the Sun, the mechanisms of angular-momentum redistribution, and theworkings of the solar dynamo. The first two were of general interest to thebroad scientific community beyond astronomy, and were, quite rightly,principally responsible for our acclaimed success; the others are still in astate of flux.

What have we learned from helioseismology, what have we really learned, and what do we aspire to learn?