Abundances can be evaluated using the DEM (Differential Emission Measure)
technique.  We refer the reader to Parenti et al. (2000, Astron. Astrophys.,
363, 800) for a description of the method.  The log of the DEM is plotted
versus the log of the electron temperature T, from CDS and UVCS data for
the equatorial and mid-latitude streamers of March 8, 1998 (shown in the
previous figure).  Scarcely any FIP effect shows up in CDS data; a
depletion of oxygen, larger than that found for low FIP elements, is
clearly derived from UVCS data; the abundance of all elements decreases
with height.  The curves give also some indication about the plasma
temperature.  We point out that the plasma is practically isothermal,
both at the CDS and UVCS levels.  A temperature versus altitude profile
is given in the next figure.