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Yushchenko, Alexander,Doikov, Dmytry,Andrievsky, Sergei,Jeong, Yeuncheol,Yushchenko, Volodymyr,Rittipruk, Pakakaew,Kovtyukh, Valery,Demessinova, Aizat,Gopka, Vira,Raikov, Alexander,Jeong, Kyung Sook The Korean Space Science Society 2022 Journal of astronomy and space sciences Vol.39 No.4
We investigated the chemical composition of the planetary host halo star HD47536 via high-resolution spectral observations recorded using a 1.5 meter Cerro Tololo Inter-American Observatory (CTIO) telescope (Chile). Furthermore, we determined the abundances of 38 chemical elements. Both light and heavy elements were overabundant compared to the iron group elements. The abundance pattern of HD47536 was similar to that of halo-type stars, with an enrichment of heavy elements. We analyzed the relationships between the relative abundances of chemical elements and their second ionization potentials and condensation temperatures. We demonstrated that the interplay of charge-exchange reactions owing to the accretion of interstellar matter and the gas-dust separation mechanism can influence the initial abundances and can be used to qualitatively explain the abundance patterns in the atmosphere of HD47536.
Alexander Yushchenko,Dmytry Doikov,Sergei Andrievsky,Yeuncheol Jeong,Volodymyr Yushchenko,Pakakaew Rittipruk,Valery Kovtyukh,Aizat Demessinova,Vira Gopka,Alexander Raikov,Kyung Sook Jeong 한국우주과학회 2022 Journal of Astronomy and Space Sciences Vol.39 No.4
We investigated the chemical composition of the planetary host halo star HD47536 via high-resolution spectral observations recorded using a 1.5 meter Cerro Tololo Inter-American Observatory (CTIO) telescope (Chile). Furthermore, we determined the abundances of 38 chemical elements. Both light and heavy elements were overabundant compared to the iron group elements. The abundance pattern of HD47536 was similar to that of halo-type stars, with an enrichment of heavy elements. We analyzed the relationships between the relative abundances of chemical elements and their second ionization potentials and condensation temperatures. We demonstrated that the interplay of charge-exchange reactions owing to the accretion of interstellar matter and the gas-dust separation mechanism can influence the initial abundances and can be used to qualitatively explain the abundance patterns in the atmosphere of HD47536.
Chemical Composition of RM_1-390 - Large Magellanic Cloud Red Supergiant
Alexander V. Yushchenko,정연철,Vira F. Gopka,Svetlana V. Vasil’eva,Sergey M. Andrievsky,Volodymyr O. Yushchenko 한국우주과학회 2017 Journal of Astronomy and Space Sciences Vol.34 No.3
A high resolution spectroscopic observation of the red supergiant star RM_1-390 in the Large Magellanic Cloud was made from a 3.6 m telescope at the European Southern Observatory. Spectral resolving power was R=20,000, with a signal-to-noise ratio S/N > 100. We found the atmospheric parameters of RM_1-390 to be as follows: the effective temperature Teff = 4,250 ± 50 K, the surface gravity log g = 0.16 ± 0.1, the microturbulent velocity vmicro = 2.5 km/s, the macroturbulence velocity vmacro = 9 km/s and the iron abundance [Fe/H] = -0.73 ± 0.11. The abundances of 18 chemical elements from silicon to thorium in the atmosphere of RM_1-390 were found using the spectrum synthesis method. The relative deficiencies of all elements are close to that of iron. The fit of abundance pattern by the solar system distribution of r- and s-element isotopes shows the importance of the s-process. The plot of relative abundances as a function of second ionization potentials of corresponding chemical elements allows us to find a possibility of convective energy transport in the photosphere of RM_1-390.