N-IV EMISSION-LINES IN THE ULTRAVIOLET-SPECTRA OF GASEOUS NEBULAE

Theoretical electron density sensitive emission-line ratios, determine d using electron impact excitation rates calculated with the R-matrix code, are presented for R = I(2s2 1S-2s2p 3P2)/I(2s2 1S-2s2p 3P1) = I( 1483 angstrom)/I(1486 angstrom) in N IV. These are found to be up to a n order of magnitude different from those deduced by previous authors, principally due to the inclusion of excitation rates for transitions among the 2s2p 3P fine-structure levels. The observed values of R for several planetary nebulae, symbiotic stars and the Cygnus Loop superno va remnant, measured from spectra obtained with the International Ultr aviolet Explorer (IUE) satellite and the Hopkins Ultraviolet Telescope (HUT), lead to electron densities which are in excellent agreement wi th those deduced from line ratios in other species. This provides obse rvational support for the accuracy of the atomic data adopted in the p resent calculations.