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The analysis of Li I 6708A line was performed for 6 rotational phases distributed over the whole rotational period (9.5 years) of HD166473. The magnetic field model was constructed based on the polarimetric measurements from (Mathys et al. 20007). For each observed phase the modulus of the magnetic field was also estimated from simulation of the Fe II 6147A, 6149A and Pr III 6706.7A line profiles taking into account Zeeman magnetic splitting. The lithium abundance in each phase was obtained from fitting the observed Li I 6708A profile with the synthetic one calculated assuming Paschen-Back splitting and estimated magnetic field characteristics from Pr III 6706.7A line profile., Comment: 2 pages 1 figure, IAU 302 "Magnetic fields throughout stellar evolution"

The obvious lack of the binary stellar systems that contain neutron stars (NS) is observed at present. Partly it is caused by the fact that it is very difficult to detect neutron star in a binary system if this relativistic component does not manifest itself as a radio pulsar. Among 1879 pulsars that are listed in the ATNF pulsar catalogue, only 141 pulsars are known to be the companions in binary systems. Only 81 objects having median mass estimation of more than 0.2 $M_{\odot}$ constitute the binary systems with pulsars. Nevertheless, such systems should be much more numerous and their investigation is of the great interest because thier structure and evolution can certainly help in our understanding of many unique properties that are seen in some stars., Comment: Accepted to published in the Odessa Astronomical Publications, 2012, vol. 25/1, p.35-39

Ground-level ozone in Kiev for an episode of its high concentration in August 2000 was simulated with the model of the urban air pollution UAM-V (Urban Airshed Model). The study of total ozone over Kiev and its concentration changes with height in the troposphere is made on the basis of ground-based observations with the infrared Fourier spectrometer at the Main Astronomical Observatory of National Academy of Sciences of Ukraine as a part of the ESA-NIVR-KNMI no 2907. In 2008 the satellite Aura-OMI data OMO3PR on the atmosphere ozone profiles became available. Beginning in 2005, these data include the ozone concentration in the lower layer of the atmosphere and can be used for the evaluation of the ground-level ozone concentrations in all cities of Ukraine. Some statistical investigation of ozone air pollution in Kiev and medical statistics data on respiratory system was carried out with the application of the "Statistica" package. The regression analysis, prognostic regression simulation, and retrospective prognosis of the epidemiological situation with respect to respiratory system pathologies in Kiev during 2000-2007 were performed., Comment: 8 pages, 3 figures, 1 table, published in Kosmichna Nauka i Tekhnologiya (ISSN 1561-8889), 2011, Vol. 17, No. 1, p. 52-59

We discuss some statistical results on the evolution of magnetic CP stars in the framework of the supposition about their binary nature., Comment: 3 pages, 3 figures

The study of total ozone columns above Kiev and variations of ozone concentrations in the troposphere at different altitudes above Kiev was carried out using ground-based Fourier Transform InfraRed (FTIR) spectrometric observations that are taken on a routine basis at the Main Astronomical Observatory of the National Academy of Sciences of Ukraine (MAO NASU). This study was performed within the framework of the international ESA-NIVR-KNMI OMI-AO project no.2907 entitled OMI validation by ground-based remote sensing: ozone columns and atmospheric profiles during the time frame 2005-2008. The infrared FTIR spectral observations of direct solar radiation in the wavelength range of 2-12 micron as transmitted through the Earth's atmosphere were performed during the months of April-October of each year. The aim of the project was the validation of total ozone columns and vertical ozone profiles as obtained by the Ozone Monitoring Instrument (OMI)) onboard of the NASA EOS-Aura scientific satellite platform. The modeling of the ozone spectral band shape near 9.6 microns was performing with the MODTRAN code and a molecular band model based on the HITRAN-2004 molecular database. The a-priori information for the spectral modeling consisted of water vapor and temperature profiles from the NASA EOS-Aqua-AIRS satellite instrument, stratospheric ozone profiles from the NASA EOS-Aura-MLS satellite instrument, TEMIS-KNMI climatological ozone profiles and surface ozone concentration measurements performed at the specific times of infrared spectra observations. The troposphere ozone variability was analyzed for two typical episodes: the spring episode of enhanced total ozone columns and the summer episode of enhanced surface ozone concentrations., Comment: 15 pages, 9 figures, published in Kosmichna Nauka i Tekhnologiya (in russian), 2010, Vol. 16, No. 4, p. 3-12

We report on ground-based FTIR observations being performed within the framework of the ESA-NIVR-KNMI project 2907 entitled "OMI validation by ground based remote sensing: ozone columns and atmospheric profiles" for the purpose of OMI data validation. FTIR observations were performed during the time frames August-October 2005, June-October 2006 and March-October 2007, mostly under cloud free and clear sky conditions and in some days from early morning to sunset covering the full range of solar zenith angles possible. Ozone column and ozone profile data were obtained for the year 2005 using spectral modeling of the ozone spectral band profile near 9.6 microns with the MODTRAN3 band model based on the HITRAN-96 molecular absorption database. The total ozone column values retrieved from FTIR observations are biased low with respect to OMI-DOAS data by 8-10 DU on average, where they have a relatively small standard error of about 2%. FTIR observations for the year 2006 were simulated by MODTRAN4 modeling. For the retrieval of ozone column estimates and particularly ozone profiles from our FTIR observations, we used the following data sources to as input files to construct the (a priori) information for the model: satellite Aqua-AIRS water vapor and temperature profiles; Aura-MLS stratospheric ozone profiles (version 1.5), TEMIS climatological ozone profiles and the simultaneously performed surface ozone measurements. Ozone total columns obtained from our FTIR observations for year 2006 with MODTRAN4 modeling are matching rather well with OMI-TOMS and OMI-DOAS data where standard errors are 0.68% and 1.11%, respectively. AURA-MLS data which have become available in 2007 allow us to retrieve tropospheric ozone profiles., Comment: 13 pages, 6 figures, 1 table, pablished in Kosmichna Nauka i Tekhnologiya (ISSN 1561-8889), Vol. 14, No. 5, p. 85 (2008)

The magnetic star HD 21699 possesses a unique magnetic field structure where the magnetic dipole is displaced from the centre by 0.4 +/- 0.1 of the stellar radius (perpendicularly to the magnetic axis), as a result, the magnetic poles are situated close to one another on the stellar surface with an angular separation of 55$^o$ and not 180$^o$ as seen in the case of a centred dipole. Respectively, the two magnetic poles form a large "magnetic spot". High-resolution spectra were obtained allowing He I and Si II abundance variations to be studied as a function of rotational phase. The results show that the helium abundance is concentrated in one hemisphere of the star, near the magnetic poles and it is comparatively weaker in another hemisphere, where magnetic field lines are horizontal with respect to the stellar surface. At the same time, the silicon abundance is greatest between longitudes of 180 - 320$^o$, the same place where the helium abundance is the weakest. These abundance variations (with rotational phase) support predictions made by the theory of atomic diffusion in the presence of a magnetic field. Simultaneously, these result support the possibility of the formation of unusual structures in stellar magnetic fields. Analysis of vertical stratification of the silicon and helium abundances shows that the boundaries of an abundance jump (in the two step model) are similar for each element; $\tau_{5000}$ = 0.8-1.2 for helium and 0.5-1.3 for silicon. The elemental abundances in the layers of effective formation of selected absorption lines for various phases are also correlated with the excitation energies of low transition levels: abundances are enhanced for higher excitation energy and higher optical depth within the applied model atmosphere., Comment: accepted by MN, 7 pagers, 10 figs, 3 tables

We analyse the spectral energy distribution of the evolved carbon giant DY Per with a spectral synthesis technique. The red giant shows the photometric features of R CrB type stars. We derive the atmospheric parameters of DY Per using three variants of molecular line lists. We estimate Teff to be in the range 2900 < Teff < 3300 K. We adopted log g = 0. The star may be metal deficient and hydrogen deficient. The maximum possible carbon abundance in the star, [C]=0.94, provides the following atmospheric parameters: Tef=3100 K, [Fe/H] = 0, log(C/O)=0.6, [N/Fe] = 0, [H/He] = 0, with Jorgensen's line lists for the molecules C2 and CN., Comment: 4 pages, 2 tables, 3 figs, accepted by Odessa asronomical observatory Publ., 2009

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 A, using a most complete line list including all possible transitions between REE levels of NIST database. Our model calculations were performed under two assumptions: blend of Li and REE lines, and blend of REE lines only. They prove that Li lines are present in the range 6707.72-6708.02 AA, and that the resulting Li abundance is 3.1 dex (in the scale log N(H) = 12.0, while the isotopic ratio 6Li/7Li is near to 0.3., Comment: 8 pages, 2 figs, 4 tables, accepted by AA

We present the results of the observations of some roAp stars made at Mount Stromlo Observatory during 17 nights in 2001 September-October. This long observing run permitted us to obtain a good phase-rotation coverage. In chemically peculiar magnetic stars, the Li I 6708 A spectral line presents very anomalous behaviour: in some stars it is a strong feature, in others, with similar atmospheric parameters, it is invisible. Interesting results were obtained for the roAp star HD 3980 which presents variations of the profile and position of the Li I line with the rotation period. These new observational results should serve as a base for the development of atmospheric models of ``Li-spotted'' roAp stars., Comment: 13 pages, LaTeX, 7 figures, newpasp.sty. To appear in the proceedings of the IAU Symposium 210 "Modelling of Stellar Atmospheres", eds. N.E. Piskunov, W.W. Weiss, D.F. Gray