SPECTRAL-LINES FROM SOURCE REGIONS OF THE SOLAR-WIND - THE O-VI RESONANCE DOUBLET

We present numerical simulations of intensities and profiles of the O VI lambda1032 and lambda1038 lines expected from an equatorial and pol ar coronal hole at solar minimum, when observed on the plane of the sk y in the 1.2 R.-8 R. range of heliocentric distance. The radial variat ions of coronal temperatures, densities and outflow speeds inside thes e structures are those determined by Withbroe (1988) through a one-flu id steady-state radiative energy balance model. We discuss how the spe ctral features depend on the physical parameters of the examined struc tures, in order to evaluate to which extent they can put constraints o n empirical models of the extended solar corona. These results may con tribute to prepare and interpret SPARTAN and UVCS/SOHO future observat ions.