Emission lines from very highly ionized iron have been observed
during solar flares. The UVCS range includes
[Fe XVIII] 
974.9, [Fe XIX] 
1118.1,
and [Fe XXI] 
1354.0, which are formed at log T = 6.8, 6.9
and 7.0, respectively. The aim of this proposal is to observe
material ejected by flares and investigate the spatial distribution
of very hot material above the flare. Line shape and shifts in
the different parts of the source will allow mapping of the strong
non-thermal velocity components which are expected in these events.
We will determine if hot plasma is observed, its spatial distribution
and the upper limit of the region where hot material can be formed and
transported in the corona. Hot plasma can be ejected at high velocity
during flare phenomena in association with the impulsive phase. The Hard
X-ray Imaging Spectrometer on SMM showed that very extended post-flare
loops develop in the corona at the end of very intense flares. They
expand at least up to 1.3 
,
maintaining flare temperatures (
10
K) and relatively high
density (2.5 10
cm
).
