Abstract
The analysis of high resolution spectra of the HgMn star HD 216494 recorded by the SWP camera on board the International Ultraviolet Explorer reveals no variations of the far-ultraviolet flux of this star over 2 days in 1995 July. The far-ultraviolet resonance lines of Si ii are strong absorbers in the spectrum of HD 216494. The resonance lines of Ga ii, Ga iii and Hg ii, characteristic of classical HgMn stars, are also present in the mean SWP spectrum of HD 216494. The currently available TESS lightcurves of HD 216494 has a double wave structure with a period between two successive deep minima equal to 3.486 ± 0.054 days which could be the rotation period.
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