Origins of the slow and the ubiquitous fast solar wind

Details Origins of the slow and the ubiquitous fast solar wind Origins of the slow and the ubiquitous fast solar wind

1997-09-03

arxiv.org/abs/astro-ph/9709021v1

Astronomy and Astrophysics

Astrophysics

15 pages, LaTex, 6 jpg figures, accepted Aug. 28, 1997 for publication in the ApJ Letters

Scientific paper

10.1086/310970

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.

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