The accompanying figure shows images of the 12 February 2000 flux rope
Coronal Mass Ejection images from LASCO/SOHO and UVCS/SOHO.  The
white-light image on the left was taken with the LASCO C2 coronagraph.
The position of the UVCS entrance slit during this event (2.3 solar
radii) is indicated in the LASCO image.

On the right side of the figure are time-lapse images of the intensity
(top) and Doppler shift velocity (bottom) of the H I Lyman alpha spectral
line, as it evolved over a period of about 10 hours.  Time has been
converted into radius by taking account of the overall bulk speed of
the CME.

The Lyman alpha images show the same general morphology as the LASCO
images.  The first material to pass through the slit is the bright
compression front.  That is followed by a low-intensity cavity, then
the bright prominence material passes through the slit.  UVCS detected
emission from lines of hydrogen, oxygen, silicon, and carbon in this
CME.  Line widths and intensities provide information about proton,
electron, and ion temperatures, bulk 3D flows, elemental abundances, 
the ionization state of the plasma, and its helicity (the handedness
and geometry of the twisted magnetic field).

The Doppler shift of these spectral lines shows the velocity component
along the line of sight of the different part of the CME.  In the
Doppler shift image, white represents zero line-of-sight velocity, dark
blue represents 83 km/sec toward the observer, and dark red represents
44 km/sec away from the observer.  The brightest part of the front
(on the lower right) is less blue-shifted than the upper-left part,
and the trailing prominence material shows a more structured Doppler
shift pattern. The Doppler dimming of O VI lines indicates an outflow
speed greater than 100 km/sec.

(Ciaravella et al. 2001, in preparation)