Measurement of the spectrum of plasma waves in the solar corona is needed in order to answer questions on the nature of the plasma turbulence and energy transfer responsible for the high coronal temperatures. In planned solar probe missions, wave measurements at low frequency are important for understanding magnetohydrodynamic heating processes of the corona. Higher frequency plasma waves provide a relatively sensitive signature of the kinetic processes that may be involved in the heating, transport, and acceleration of particles. Because there have been no in situ measurements of the solar corona, the spectrum of plasma waves cannot be precisely predicted; however, experience with solar wind and magnetospheric experiments suggests that the very dynamic nature of the corona must lead to a wide range of plasma wave emissions. Indeed, the dynamic spectra of solar radio bursts received at earth are an indication that many plasma emission processes occur in the corona. It is therefore suggested that the plasma wave spectrum up to and above the local plasma frequency should be measured during future in situ missions. We discuss this approach to planned solar probe missions and suggest some of the experimental results that may be achieved. ©1997 American Institute of Physics.