THE ULTRAVIOLET-SPECTRUM OF KX-TRIANGULI AUSTRALIS

The symbiotic star KX TrA (= Cn 1-2) was observed with the IUE satellite in the low- and high-dispersion mode on 1990 May 7. The low-dispersion data show no significant changes from previous observations taken a decade ago. The high-dispersion spectra were used to determine electron densities from several diagnostic line ratios and show a range of log N(e) from 5.8 to 11.1 cm-3. No P Cygni-type features were observed. Resonantly excited high-excitation Fe II emission lines are seen in the UV spectrum of KX TrA, which strongly argues for the existence of a very hot (> 60,000 K) subdwarf or white dwarf in the system. As was previously noted, the S-type symbiotic KX TrA exhibits an UV spectrum that is nearly identical to that of the D-type symbiotic V1016 Cyg.