2016AstBu..71..199Z

The axial rotation of a star plays an important role in its evolution, the physical conditions in its atmosphere and the appearance of its spectrum. We analyzed the CCD spectra of two stars for which their projected rotational velocity differs remarkably when derived from Ca II 3933 A and Mg II 4481 A lines. We estimated the projected rotational velocity of HD182255 to be 15.5 km/s, although in various spectra of this star the line widths correspond to values as high as 28.5 km/s. We found the HeI 4471.498 A line to be shifted to longer wavelengths by 0.046 A, thus indicating a presence of the 3He I: 4He ratio from 0.2 to 0.6.We also found an absorption feature at the position of the forbidden line He I 4470.02. We found the lines of Mg II and CII originating from higher excited levels to be missing in the spectra of HD 182255. For HD 214923 we determined the projected rotational velocity v sin i=165km/s from the profiles of the metallic lines and Ca II 3933A, whereas for helium lines v sin i ∼ 130km/s is more appropriate. Radial velocity analysis results in three long periods of ∼ 105, 34, and 15 days, and a short period of ∼ 22 hours, close to the pulsational one mentioned earlier in the literature.