Electron density and temperature of the lower solar corona

Off limb observations of the quiet Sun corona were made with the Coronal Di agnostic Spectrometer (CDS) on SOHO during the Whole Sun Month campaign in August 1996. Selected spectral lines in the Normal Incidence range were rec orded up to 1.2 solar radii above the east and west limb and above the pola r coronal holes. Intensities of the coronal lines covering the temperature range from 9x10(5) to 2x10(6) K have been measured and used to derive elect ron temperature and electron density as a function of the radial distance a bove the solar limb. Results from the east and west equatorial regions and polar coronal holes are compared. The temperature and density in the corona l holes is found to be lower than in the closed field regions. A density-se nsitive line ratio of Si IX 350/342 Angstrom is used to derive an average e lectron density which is found to decrease from 5 x 10(8) cm(-3) near the l imb to 1 x 10(8) cm(-3) at 1.15R(S), in the equatorial region. Over the pol ar coronal holes, where polar plumes dominate the emission close to the lim b, the density varies from 2 x 10(8) cm(-3) at the limb to 6 x 10(7) cm(-3) at 1.1R(S). The lowest density found inside the coronal hole on the disk i s 9.9 x 10(7) cm(-3). An increase in the quiet Sun temperature with the rad ial distance is found from the Si XII/Mg X and Si XII/Mg IX line ratios, an d an increase in the coronal hole temperature is seen from the Mg X/Mg IX r atio. The Si XII/Mg X temperature varies from 1.1 x 10(6) K at r = R-S to 1 .4 x 10(6) K at r = 1.2R(S) in the equatorial regions. The EUV emission is compared with that of the soft X rays as measured by the Yohkoh SXT. The de nsities and temperatures determined from the SXT show a similar behavior to that determined from the CDS. Density and temperature, averaged over a pos ition angle range of 20 - 54 degrees, show very little variation over a per iod of 20 days.