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Presence of MG II emission in R CrB at maximum light.
Kameswara-Rao, N.; Nandy, K.; Bappu, M. K. V.
The high dipersion spectrum of R CrB in the long wavelength obtained near its maximum with the International Ultraviolet Explorer shows the presence of chromospheric Mg II emission. For comparison the spectrum of Gamma Cyg was obtained immediately afterwards. The Mg II emission width of R CrB is found to be the same as that of Gamma Cyg.
Analysis of IUE observations of the galactic corona and the existence of molecular clouds in the halo
Hartquist, T. W.; Tallant, A.
IUE observations of ions in the galactic corona are reanalyzed and Savage and de Boer's (1979) conclusion that the detected hot phase has a temperature proportional to 80,000 K is confirmed. The cold phase must be at a temperature of less than 24,000 K and probably contains substantial amounts of molecular material. Molecules, such as CH(+), OH an…
Anomalous far-uv extinction in the WN 6 star HD 147419.
Willis, A. J.; Stickland, D. J.
IUE observations of two WN stars in ring nebulae, HD 147419 and HD 89358, show that in the former star, the level of far UV interstellar extinction, λ > 1600 Å, is far higher than expected from the mean galactic extinction law. The derived scale of extinction for HD 147419, Aλ/EB-V, agrees well with the mean galactic law at λ > 16…
IUE observations of high-velocity components in spectra of beta Orionis.
Bates, B.; Giaretta, D. L.; Brown-Kerr, W.
The high dispersion spectrum of R CrB in the long wavelength obtained near its maximum with the International Ultraviolet Explorer shows the presence of chromospheric Mg II emission. For comparison the spectrum of γ Cyg was obtained immediately afterwards. The Mg II emission width of R CrB is found to be the same as that of γ Cyg.
Molecules in celestial objects. II. IUE observations of CO towards psi Per (B5 Ve).
Tarafdar, S. P.; Swamy, K. S. K.
Absorption features corresponding to 1-0, 2-0, 3-0 and 4-0 bands of the A-X transition of CO have been identified in the spectra of a hot shell star, Psi Per (B5 Ve, E(B-V)=0.09). Arguments are put forward to suggest its possible origin in the circumstellar shell.