Observing the Influence of Alfven Waves on the Energetics of the Quiet Solar Corona and Solar Wind

We will present and discuss recent observations of Alfvén waves in the solar chromosphere, from the Solar Optical Telescope (SOT) on Hinode, and in the corona, from HAO's ground-based Coronal Multi-channel Polarimeter (CoMP). These observations unambiguously demonstrate, for the first time, that the magnetic chromosphere and corona are riddled with 3- and 5-minute (3-5mHz) Alfvénic oscillations predominantly propagating outward into the heliosphere. The combined analysis of these observations, augmented by spectroscopic data from SOHO/SUMER, provide a compelling look at the influence and importance of ubiquitously driven Alfvén waves in heating the quiet solar corona and driving the solar wind. Indeed, we believe that these direct observations of a low-frequency wave input must provoke a re-evaluation of solar wind acceleration by high frequency (kHz) ion-cyclotron modes.