  We present in this Letter the first coordinated radio occultation
measurements and ultraviolet observations of the inner corona below 5.5 Rs,
obtained during the Galileo solar conjunction in January 1997, to establish the
origin of the slow solar wind. Limits on the flow speed are derived from the
Doppler dimming of the resonantly scattered componentof the oxygen 1032 A and
1037 A lines as measured with the UltraViolet Coronagraph Spectrometer (UVCS)
on the Solar and Heliospheric Observatory (SOHO). White light images of the
corona from the Large Angle Spectroscopic Coronagraph (LASCO) on SOHO taken
simultaneously are used to place the Doppler radio scintillation and
ultraviolet measurements in the context ofcoronal structures. These combined
observations provide the first direct confirmation of the view recently
proposed by Woo and Martin (1997) that the slow solar wind is associated with
the axes, also known as stalks, of streamers. Furthermore, the ultraviolet
observations also show how the fast solar wind is ubiquitous in the inner
corona, and that a velocity shear between the fast and slow solar wind develops
along the streamer stalks.
