  This paper reviews the latest observational evidence for the existence of
propagating waves in the open magnetic flux tubes of the solar corona. SOHO
measurements have put tentative limits on the fluxes of various types of
magnetohydrodynamic (MHD) waves in the acceleration region of the solar wind.
Also, continually improving measurements of fluctuations at larger distances
(i.e., in situ detection and radio scintillation) continue to provide
significant constraints on the dominant types of plasma oscillation throughout
the corona and wind. The dissipation of MHD fluctuations of some kind, probably
involving anisotropic turbulent cascade, is believed to dominate the heating of
the extended corona. Spectroscopic observations from the UVCS instrument on
SOHO have helped to narrow the field of possibilities for the precise modes,
generation mechanisms, and damping channels. This presentation will also review
some of the collisionless, kinetic aspects of wave heating and acceleration
that are tied closely to the observational constraints.
