Abstract
The analysis of low and high resolution spectra of the late B-type star HD 179761 recorded by the SWP camera on board the International Ultraviolet Explorer reveals no variations of the far ultraviolet flux of this star in 1983 May and June. The far ultraviolet resonance lines of Si ii are strong absorbers in the spectrum of HD 179761. The resonance lines of Ga ii, Ga iii and Hg ii, characteristic of clasical HgMn stars, do not seem to be present in the mean SWP spectrum of HD 179761. The currently available TESS lightcurves of HD 179761 suffer from data dropouts and suggest low amplitude variations with periods runing from 4.86 to 5.44 days which need confirmation.
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