Abstract
The analysis of low and high resolution spectra of the chemically peculiar stars HD 53929 and HD 172044 recorded by the SWP camera on board the International Ultraviolet Explorer reveals no variations of the far-ultraviolet fluxes of these stars. The far-ultraviolet Ga ii and Ga iii resonance lines are strong absorbers in the spectrum of HD 172044. The TESS lightcurve of HD 172044 suggests a period close to 4.347 ± 0.135 days which could be the rotational period. On SWP 34118 the resonance lines of Si ii and Ga ii are blueshifted compared to SWP 34110 probably reflecting the orbital motion of HD 172044.
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