DENSITY AND TEMPERATURE DIAGNOSTICS OF SOLAR EMISSION-LINES FROM NE(VI) AND MG(VI)

Line intensity ratios of NeVI lines with respect to a resonance line o f MgVI have been considered for electron density and temperature deter minations within the chromosphere-corona transition region. The electr on pressure within the transition region has been assumed to be consta nt. In addition, these ratios would enable us to estimate the relative element abundances of neon to magnesium. An attempt has been made to explain the extreme ultraviolet intensities of NeVI and MgVI lines as observed by ATM ultraviolet spectrometer. The observed intensities cor respond to the average quiet-Sun conditions near solar minimum. Theore tical intensities for NeVI and MgVI lines have been computed using a m odel solar atmosphere. Theoretical intensities obtained by using the v alues 3.98 x 10(-5) and 3.16 x 10(-5) for element abundance of Ne and Mg, respectively, seem to agree well with the expected intensities. Th e agreement between some of the expected and computed intensities sugg ests the need for future observations at higher spectral resolutions t o resolve difficulties arising out of blending due to two or more line s.