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Understanding the physical processes responsible for accelerating the solarwind requires detailed measurements of the collisionless plasma in the extendedsolar corona. Some key clues about these processes have come from instrumentsthat combine the power of an ultraviolet (UV) spectrometer with an occultedtelescope. This combination enables measurements of ion emission lines far fromthe bright solar disk, where most of the solar wind acceleration occurs.Although the UVCS instrument on SOHO made several key discoveries, manyquestions remain unanswered because its capabilities were limited. This whitepaper summarizes these past achievements and also describes what can beaccomplished with next-generation instrumentation of this kind.

Ultraviolet Coronagraph Spectroscopy: A Key Capability for Understanding the Physics of Solar Wind Acceleration