  Helioseismology has taught us a great deal about the stratification and
kinematics of the solar interior, sufficient for us to embark upon dynamical
studies more detailed than have been possible before. The most sophisticated
studies to date have been the very impressive numerical simulations of the
convection zone, from which, especially in recent years, a great deal has been
learnt. Those simulations, and the seismological evidence with which they are
being confronted, are reviewed elsewhere in this volume. Our understanding of
the global dynamics of the radiative interior of the Sun is in a much more
primitive state. Nevertheless, some progress has been made, and seismological
inference has provided us with evidence of more to come. Some of that I
summarize here, mentioning in passing hints that are pointing the way to the
future.
