2025RNAAS...9....6M

The weak line of Hg II located at 5677.10 Å is not detected in Ultraviolet and Visible Echelle Spectrograph spectra of the Chemically Peculiar star HR 6000. This is explained by the very low mercury excess in this young late B-type star. The synthesis of various spectral intervals yields several new measurements of the abundances of helium, carbon, oxygen, magnesium, aluminium, silicon, phosphorus, titanium, chromium, manganese, iron, nickel, gallium, yttrium and xenon. Helium is found to be very depleted by -2.0 dex, most of the other measurements agree with the abundances previously published. An examination of the Transiting Exoplanet Survey Satellite light curves of HR 6000 shows that the optical flux is variable on timescales of days but no clear periodicity is visible.