In view of the preparation and interpretation of UVCS/SOHO future
observations, it is important
to estimate the EUV emission line intensities and profiles
to be expected in coronal structures
to be observed by this instrument.
In this chapter we give some estimates of the intensity values
expected for UVCS/SOHO observations of HI Ly-
and OVI
1032
and 
1037, obtained as a function
of heliocentric distance for different regions in the extended solar corona.
To calculate the line intensities, we have used models which specify the plasma temperatures, densities and outflow velocities in coronal holes. In this context, it should be kept in mind that there are relatively few empirical values of these quantities for the extended solar corona. As the line intensities depend strongly on the assumed plasma parameters, they are intended only for order-of-magnitude estimates.
Section 3.2 provides intensity values for HI Ly-
and OVI in
coronal holes. In section 3.2.1 we
give the expression used to calculate
the intensities and the assumed atomic data
for the HI and OVI lines. In section 3.2.2 we describe the
densities, velocities and temperatures assumed
for the coronal regions considered. The results for the line
intensities calculated using the assumptions
described in sections 3.2.1 and 3.2.2 are reported in
section 3.2.3. Section 3.2.4 provides measured
HI Ly-a intensities from sounding rocket and
Spartan 201 flights, and a comparison to the calculated
intensities. Section 3.3 provides measured streamer intensities for
HI Ly-a from Spartan 201 and
streamer intensities for OVI 
1032 which are scaled from the calculated coronal hole values. Section 3.4
provides a formula for deriving count rates from the
estimated intensities and also provides some examples of
the expected count rates.