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This paper reviews our growing understanding of the physics behind coronalheating (in open-field regions) and the acceleration of the solar wind. Manynew insights have come from the last solar cycle's worth of observations andtheoretical work. Measurements of the plasma properties in the extended corona,where the primary solar wind acceleration occurs, have been key todiscriminating between competing theories. We describe how UVCS/SOHOmeasurements of coronal holes and streamers over the last 14 years haveprovided clues about the detailed kinetic processes that energize both fast andslow wind regions. We also present a brief survey of current ideas involvingthe coronal source regions of fast and slow wind streams, and how these changeover the solar cycle. These source regions are discussed in the context ofrecent theoretical models (based on Alfven waves and MHD turbulence) that havebegun to successfully predict both the heating and acceleration in fast andslow wind regions with essentially no free parameters. Some new resultsregarding these models - including a quantitative prediction of the lowerdensity and temperature at 1 AU seen during the present solar minimum incomparison to the prior minimum - are also shown.

Extended Coronal Heating and Solar Wind Acceleration Over the Solar Cycle