Solar Physics Division Meeting 2000, June 19-22
Session 2. Corona, Solar Wind, Flares, CMEs, Solar-stellar, Instrumentation, Other
Display, Chair: J. Krall, Monday-Thursday, June 19, 2000, 8:00am-6:00pm, Forum Ballroom

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[2.71] SOHO/UVCS Observations of a Coronal Jet During the Third Whole Sun Month Campaign

Y.-K. Ko, J. Raymond (Harvard-Smithsonian Center for Astrophysics), S. Gibson (University of Cambridge), L. Strachan (Harvard-Smithsonian Center for Astrophysics), D. Alexander, L. Fletcher (Lockheed-Martin ATC, Solar and Astrophysics Laboratory), T. Holzer, H. Gilbert, J. Burkepile (High Altitude Observatory), C. St. Cyr (Computational Physics, Inc.), B. Thompson (NASA/GSFC)

On August 26 1999, a coronal jet occurred at the north west limb near a sigmoid active region which has been the target for a joint observation plan during the third Whole Sun Month Campaign. This jet was observed by several instruments at the limb (SOHO/CDS, SOHO/EIT, TRACE, MLSO/CHIP, MLSO/PICS), at 1.7 Ro (SOHO/UVCS), and at the outer corona (SOHO/LASCO). At 1.7 Ro, the intensities of Lyman alpha, Lyman beta in the jet increased by as large a factor of 100 compared with the background corona, while those for O VI 1032 and O VI 1037 increased by a factor of 2. C III 977 line also brightened significantly. The line shift in the lines indicates that the line-of-sight velocity in the jet started from ~150 km/sec blue shift and ended at ~120 km/sec red shift. This line-of-sight motion seen at 1.7 Ro apparently was opposite that observed when the jet emerged from the limb. In this paper, we present the observation by SOHO/UVCS and discuss the dynamic structure and physical properties of this jet as it passed through 1.7 Ro. Comparisons will be shown with the observations from other instruments. This work is supported by NASA Grant number NAG5-7822.

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