Abstract. We report the abundance determination in the atmosphere of the bright halo star HD 221170. The spectra were taken with the Terskol Observatory's 2.0-m telescope with a resolution R = 45 000 and signal-to-noise ratio up to 250 in the wavelength region 3638-10 275 Å. The adopted atmospheric parameters correspond to an effective temperature T eff = 4475 K, a surface gravity log g = 1.0, a microturbulent velocity v micro = 1.7 km s −1 , and a macroturbulent velocity v macro = 4 km s −1 . The abundances of 43 chemical elements were determined with the method of spectrum synthesis. The large overabundances (by 1 dex relative to iron) of elements with Z > 38 are shown to follow the same pattern as the solar r-abundances. The present HD 221170 analysis confirms the non-universality of the r-process, or more exactly the observation that the astrophysical sites hosting the r-process do not always lead to a unique relative abundance distribution for the bulk Ba to Hg elements, the Pb-peak elements, and the actinides.

Abstract. We carried out a detailed analysis of spectra of the unique roAp star HD 101065 (Przybylski's star) near the resonance doublet Li I 6708 Å, using a most complete line list including all possible transitions between REE levels of the NIST database. Our model calculations were performed under two assumptions: a blend of Li and REE lines, and a blend of REE lines only. They prove that Li lines are present in the range 6707.72−6708.02 Å and that the resulting Li abundance is 3.1 dex (in the scale log N(H) = 12.0), while the isotopic ratio 6 Li/ 7 Li is near to 0.3.

Abstract. As a further step in our Lithium project we present results of abundance determination of some elements in the roAp star HD 60435. Possible NLTE effects were considered. Equivalent widths of spectral lines vary with rotational phase which suggests nonuniform distribution of chemical elements over the stars' surface. Large abundance differences derived from various ions of some rare earth elements indicate their possible vertical stratification. Two spots of enhanced lithium abundance were distinguished at the magnetic poles on HD 60435 and their parameters derived. The rotational axis inclination i = 133• or 47• and surface magnetic field Hs = 3± 1 kG were determined for the first time for HD 60435. The results are compared with HD 83368, the other star with lines of lithium remarkably variable in intensity and wavelength.

Abstract. Using high-dispersion spectral observations of HD 101065 (Przybylski's star) we have identified the lines of heavy radioactive elements with atomic numbers from 84 to 99 in the spectrum of the star. We found the lines of all these elements except At (Z=85) and Fr (Z=87). We try to explain a presence of such heavy species in the atmosphere of this star as a result of radioactive decay of Th and U nuclei and neutron capture process producing some transuranium isotopes. The necessary conditions for these processes to work may appear due to atomic diffusion and favorable accumulation of the thorium and uranium nuclei in the upper of the PS atmosphere.

Abstract. An internacional project "Lithium in magnetic Ap stars" has been run since 1996 with the purpose of creating an observational database allowing systematic studies of the abnormal occurence of lithium on the surface of cool Ap stars. The 2.6 m telescope at the Crimean Astrophysical Observatory, the ESO CAT, ESO 1.52 m telescope with FEROS, the Nordic Optical Telescope, and the 74" telescope at Mount Stromlo were employed to collect observations at the regions of the lithium resonance lines λ 6103 and λ 6708Å.Observations of the roAp-stars HD 83368, HD 60435 and HD 3980 revealed considerable periodical Doppler shifts of the line of lithium λ 6708Å which can be explained by the presence of lithium spots on their surfaces. Conjunction with structures of the magnetic field is apparent.A detailed study of the blend at λ 6708Å in HD 101065 confirmed the anomalous overabundance of lithium amounting to 3.1 dex, as well as unusual isotopic ratio 6 Li/ 7 Li∼ 0.3.