Electron temperatures (top panels) and electron densities (bottom panels),
in the altitude range from 1.02 to 1.6 solar radii, for the equatorial
and mid-latitude streamers of March 8, 1998 (see previous figures).
Temperatures (derived from the line ratio technique using Fe X to Fe XIII
lines; different symbols refer to different line ratios) increase, from
1.02 to 1.19 solar radii, reach a maximum somewhere beyond this level
and then start decreasing, as the UVCS determinations (crosses) show.
This behavior is consistent with theoretical predictions.  Densities
(derived from line ratio techniques, using lines from Si IX [diamonds]
and Si X [asterisks] in the case of CDS data, and a technique based on
the separation of the radiative and collisional components of the O VI
line at 1032 Angstrom, in the case of UVCS data [crosses]) decrease
with height, following closely a hydrostatic equilibrium law.