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 polar coronal hole at solar minimum, when observed on the plane of the sky in the 1.2 R.-8 R. range of heliocentric distance. The radial variations of coronal temperatures, densities and outflow speeds inside these structures are those determined by Withbroe (1988) through a one-fluid steady-state radiative energy balance model. We discuss how the spectral features depend on the physical parameters of the examined structures, in order to evaluate to which extent they can put constraints on empirical models of the extended solar corona. These results may contribute to prepare and interpret SPARTAN and UVCS/SOHO future observations.