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L. Strachan, A. V. Panasyuk, J. L. Kohl (Harvard-Smithsonian Center for Astrophysics), A. Breen (Physics Dept., University of Wales, Aberystwyth)
We compare the plasma properties of two different streamer regions in the extended corona (1.5 to 6 solar radii) with solar wind velocity measurements made at larger distances during the Third Whole Sun Month Campaign. Ultraviolet Coronagraph Spectrometer (UVCS/SOHO) measurements were made of H Ly-alpha intensities and profiles and O VI 1032/1037 intensities in order to put constraints on the plasma conditions in these regions. The UVCS/SOHO measurements were centered at position angles 70 deg (CCW from NHP) during 12-21 Sept. 1999 and 190 deg during 22-25 Sept. 1999. Streamer kinetic temperatures and outflow velocities are compared with measurements of outflow velocities determined by EISCAT interplanetary scintillation observations at the same position angles. The EISCAT measurements showed slow flow above the streamers at 25 to 80 solar radii, with steep gradients on the boundaries as flow speeds increased above the inter-streamer regions. Comparisons of EISCAT measurements from 25-35 solar radii and UVCS/SOHO coronal measurements should cast light on the acceleration of the slow solar wind.
This work is supported by NASA under Grant NAG5-7822 to the Smithsonian Astrophysical Observatory, by the Italian Space Agency and by PRODEX (Swiss contribution).
The author(s) of this abstract have provided an email address for comments about the abstract: lstrachan@cfa.harvard.edu