IUE satellite

After the advent of the IUE satellite it became undoubtedly clear that stellar winds are also present in many CSPN (Heap, 1978 Perinotto, 1982). Detailed studies of their wind properties have been carried out by Hamann et al. (1984) and Cerruti-Sola and Perinotto (1985). Here we... 

It was interesting that a few Algols, namely, U Cep (Plavec 1983), RW Tauri (Plavec and Dobias 1983) and TT Hydrae, U Sge and UX Monocerotis (Plavec et al. 1984) were observed with the IUE satellite at principal eclipse. And on these images the resonance doublets of C IV, Si IV and N V are displayed in emission and, as far as intensities and sequence of intensities go, they behave like in the rest of the close binary systems, that is, C IV is the strongest feature of the three. 

Recent observations of Algol type binaries observed in the ultraviolet, in particular with the IUE satellite, show that some form of mass flow is occurring in virtually all of them (McCluskey and Sahade 1987). 

The evolution of the spectrum of SN 1987A in the ultraviolet was extremely rapid and unique for an SN II. For the first day or so the spectrum was dominated by broad features from 1200 to 3200 A which were unlike any previous observed supernova (Wamsteker et al. 1987, Kirshner et al. 1987). By the third or fourth day, the spectrum resembled that of previously observed SN la and SN lb. Wheeler et al. (1986) attribute the UV spectra of SN I to resonant line scattering of Fe II, and hence a similar effect is presumably at work in SN 1987A. SN 1987A faded rapidly until it could no longer be seen at short wavelengths with the IUE satellite. 

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