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The C/O abundance ratio in the planetary nebula IC 2501.
Adams, S.; Goharji, A.
The detection of a silicon carbide feature in the infrared spectrum of the planetary nebula IC 2501 suggests that the nebular envelope is carbon rich (Aitken and Roche 1982). The authors have observed IC 2501 with the IUE satellite and have combined these observations with optical measurements in order to analyse the physical conditions and abunda…
Line profile variation in delta Orionis A, IOTA Orionis A, and 15 Monocerotis.
Grady, C. A.; Snow, T. P.; Cash, W. C.
The results of a monitoring program with IUE and Einstein are presented for three stars, δ Ori A, ι Ori A, and 15 Mon. Line profile variability is observed in the UV profiles accessible to IUE and the relation between the variation in the different ions suggests that the ionization level is varying in the winds of these stars. This is consistent w…
C IV lambda 1550 emission profiles in IUE spectra of Seyfert 1 galaxies.
Stoner, R.; Ptak, R.
Using observed C IV 1550 A emission-line profiles of type 1 Seyfert galaxies obtained with the International Ultraviolet Explorer, numerical comparisons have been made of the ability of model profiles to fit the observations. It is found that simple two-component models provide better fits to observed profiles than one-component logarithmic models…
On the reality of the 2800 A interstellar absorption feature attributed to proteins
Nandy, K.; McLachlan, A.
A hot companion to MU Sagittarii : an opportunity to sound the atmosphere of a B8 IA supergiant.
Plavec, M. J.; Polidan, R. S.
It is argued that the bright supergiant star Mu Sagittarii is accompanied by a smaller and hotter star, of spectral type approximately B1.5 V. The single-line radial-velocity curve of the B8 star leads to a fairly large mass function, f(m) = 2.64 solar masses, implying that the companion should have at least 50 percent of the mass of the visible s…
Spectrophotometry of early type supergiants in the Large Magellanic Cloud.
Nandy, K.; Houziaux, L.; Thompson, G. I. +1 more
A sample of LMC supergiants ranging in type from O5 to A1 has been subjected to equivalent width measurements of major stellar features in the visible and UV spectral regions, using methods that are entirely numerical and to the greatest possible degree free from subjective estimates. LMC member results are compared with those obtained for their g…
Ultraviolet Observations of Three Classical Novae during Early Stages of Decline
Drechsel, H.; Rahe, J.; Wargau, W.
We present IUE UV spectra of the three recent classical novae N Sgr 1982, N Ser 1983, and N Mus 1983, obtained during early decline, transitional stage, and nebular phase, respectively. The line spectra are discussed. Preliminary conclusions concerning CNO over-abundances, shell geometry, and speed classes are drawn.
The interstellar lines and the energetics of the inner Doradus nebulafrom the ultraviolet spectrum of R 136a.
Feitzinger, J. V.; Hanuschik, R. W.; Schmidt-Kaler, Th.
An IUE short and long wavelength absorption line spectrum (1150 - 3000 Å) of the central superluminous object in the 30 Doradus nebula, R 136a, is analysed. Radial velocities and equivalent widths of the Magellanic interstellar components are given. The Magellanic interstellar components fall into four well-separated groups. The same groups show u…
IUE ultraviolet observations of narrow absorption components in the spectrum of dzeta Puppis.
Prinja, R. K.
Detailed IUE ultraviolet observations of multiple absorption components, observed superimposed on the Si IV λλ1393.76, 1402.77 P Cygni resonance line doublet in the O4ef star ζ Puppis, are presented. These components are observed in 16 out of 21 spectra at ≡0.75 and 0.82 of the terminal velocity over a period of three years up to 1981 and are stat…
Optical and ultraviolet study of five stars in the Pleiades open cluster
Dufton, P. L.; Younan, K. F.
Optical and ultraviolet observations of five low-reddened stars in the Pleiades open cluster have been obtained with an echelle spectrograph and the IUE satellite. The observed interstellar absorption lines have been analysed with different cloud models to estimate interstellar gas abundances for each line-of-sight. These results have been discuss…