Abstract
The analysis of high resolution spectra of the HgMn star HD 35548A recorded by the SWP camera on board the International Ultraviolet Explorer reveals no variations of the far-ultraviolet flux of this star over about 21 hr in 1981. The resonance lines of Ga ii and Ga iii, characteristic of classical HgMn stars, are salient features in the mean SWP spectrum of HD 35548A. The TESS lightcurve of the system HD 35548A and HD 35548B has an asymetric structure with a steep descent to the minimum and a slower rise to next maximum. The period, measured between two successive maxima, is close to 6.07 ± 0.09 days which could be the orbital and rotational period due to synchronization with the companion of HD 35548A.
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