A J Lazarus, J T Steinberg (MIT); D A Biesecker (Univ. of Birmingham); R J Forsyth (Imperial College); A B Galvin (Univ. of Maryland); F M Ipavich (Univ. of Maryland); S E Gibson (NASA/GSFC/NRC); A Lecinski (High Altitude Observatory); J T Hoeksema (Stanford Univ.); P Riley (LANL); L Strachan, Jr. (CfA); A Szabo (NASA GSFC); R P Lepping (NASA GSFC); K W Ogilvie (NASA GSFC); B J Thompson (NASA GSFC/ Applied Research Corp.)
Several solar wind streams having speeds in excess of 500 km/s were observed from the Wind, SOHO, and Ulysses spacecraft during the Whole Sun Month (WSM, August 10 to September 8, 1996). By assuming that the solar wind observed in the trailing edge of a high speed stream propagates radially outward from the Sun at constant speed, an apparent heliographic longitude for its source can be determined. We compare the sources determined in that manner with observations from instruments on the SOHO spacecraft. The highest speed stream is associated with the central meridian passage of a coronal hole (CH) that has a clear equatorial extension as viewed from the SOHO EUV Imaging Telescope (EIT). The magnetic field map determined by the Michelson Doppler Imager (MDI) of the Solar Oscillations Investigation shows no obvious associations other than polarity with the extent of the CH region, as might be expected since it observes photospheric rather than coronal features. The CH boundaries do seem to match fairly well with the computed locations of open field in the potential field model of the large-scale field. As of the time of preparation of this abstract, the other streams sources apparently show little association with coronal or photospheric features, though that relationship is currently under investigation.
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