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D.A. Biesecker, T.A. Kucera (SM\&A (East)), R.R. Fisher (NASA/GSFC), S.E. Gibson (Univ. of Cambridge, UK), M. Guhathakurta (CUA), D. Wang (NRL/Interferometrics)
The SPARTAN 201/WLC was used to observe the solar corona from about 20:30 UT on 98/11/01 to about 13:30 UT on 98/11/03. The SOHO/LASCO coronagraphs were operating continuously throughout this period. The range of heights in the corona covered by the SPARTAN and LASCO coronagraphs and the temporal cadence of the data allow the properties of coronal transients to be examined in greater detail than previously possible with white light data. The SPARTAN coronagraph observes in white light brightness and polarized brightness at heights of 1.3 to 5.5 solar radii. The LASCO coronagraphs observe in white light brightness and polarized brightness at heights of 2.5 to 30 solar radii. We will measure the velocity and mass of the observed coronal transients with time. There were at least 4 coronal mass ejections observed with SOHO/LASCO during the time of the SPARTAN flight. Using solar disk images as a proxy, we will correct the data for plane of the sky projection. We will explore the height at which the CME's are initiated and the heights at which they are accelerated. In addition, we will determine what fraction of the mass is in a CME when it is initiated and how much is added throughout the event.
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