Search Publications
The IUE blaze function in the MG II region.
Morossi, C.; Vladilo, G.; Allocchio, C.
To obtain reliable emission profiles of Mg II resonance lines from the IUE data it is absolutely necessary to perform a good ripple correction of the IUE net spectrum. An experimental blaze function (valid for the IUE orders from 88 to 79) has been derived as the ratio between the IUE data and those of the Copernicus satellite: in fact, the latter…
Observations of Binaries and Evolutionary Implications
De Loore, C.
Comparison of the characteristics of groups of stars in various evolutionary phases and the study of individual systems allow to make estimates of the parameters governing mass loss and mass transfer. Observations enable us in a few cases to determine geometric models for binaries during or after the mass transfer phase (disks, rings, common envel…
IUE observations of W UMA systems AE Phoenicis and TY Mensae.
Rucinski, S. M.
SWP spectra of AE Phe and TY Men are presented and discussed. The spectrum of AE Phe is typical in showing strong emission lines which originate in the chromosphere and transition region. On the basis of the strength of the He II emission line the author predicts that AE Phe should be a moderately strong X-ray source. The spectrum of TY Men is too…
Comparison of Ultraviolet Spectra from Solar Type Stars
Wamsteker, W.; Greve, A.
We compare high-resolution spectra from the Sun and the four solar-type stars 16 Cyg A, 16 Cyg B, HD 32008, HD 34411 obtained with IUE in the wavelength range 2650-2930 Å. The comparison is made for peak intensities between absorption lines. At the level of accuracy of the IUE observations, the stars 16 Cyg A, 16 Cyg B, HD 34411 are indistinguisha…
A comparison between various UV photometric systems for late-type stars.
Cacciari, C.; Wamsteker, W.; Norgaard-Nielsen, H. U. +1 more
Ultraviolet absolute photometry and spectrophotometry obtained for late-type stars with the TD1, OAO-2, ANS, and IUE satellites are compared. Strong colour effects are found in the TD1 2740 Å band, and, to a lesser extend, in the OAO-2 2980 Å band. The reason for these effects is believed to be due to red leaks in the sensitivity functions. For th…
A comparative study of the ultraviolet spectrum of hot subdwarfs.
Altamore, A.; Viotti, R.; Rossi, L.
The high and low resolution IUE spectra of four O subdwarfs (BD +75°325, BD +48°1777, BD +37°1977, BD +37°442) are analyzed. Line identification is given for the most abundant ions in the far ultraviolet. Fe V is by far the ion with the largest number of lines. Broad P Cygni profiles of the N V and C IV resonance doublets are observed in BD +37°44…
On the λ 2800 Å interstellar extinction feature
Wickramasinghe, N. C.; Karim, L. M.; Hoyle, F.
We answer our critics and confirm the reality of a feature in the interstellar extinction curve near λ 2800 Å for stars showing abnormally low graphite absorption.
Comparison of variations in the visible and ultraviolet spectra of a Centauri.
Fahey, R. P.
Equivalent-width and central depth measurements of some ultraviolet absorption lines from the spectrum of the He I spectrum variable star a Cen (HD 125823) are presented. The measurements are from 53 short-wavelength and 52 long-wavelength, high-resolution spectrographs taken with the IUE satellite over a 25d period during 1978 July and…
Ultraviolet spectroscopy of cometary comae: An update
Feldman, P. D.
Since its launch in 1978 the International Ultraviolet Explorer (IUE) satellite observatory has been used to record ultraviolet spectra of nearly two dozen comets. These observations have been applied principally to studies of the composition, chemistry and evolution of the gaseous coma and more recently, with the substantially increased data base…
Line identifications in the ultraviolet (2590-3230 A) spectrum of thehydrogen-deficient star HD 182040.
Johnson, H. R.; Ameen, M. M.; Eaton, J. A.
Identifications for absorption features detected in the ultraviolet spectrum of the hydrogen-deficient supergiant carbon star HD 182040 observed at high resolution with the IUE satellite are presented. The spectrum in this range is filled with blended lines of the iron-peak elements, with Fe I and Cr II dominating the spectrum. Spectra definitely …