{"title":"On the determination of elemental abundances in three stars","authors":"M. Mohorian, Y. Pavlenko","doi":"10.17721/2227-1481.11.8-12","DOIUrl":null,"url":null,"abstract":"We analysed spectra of HD 126535 (K1 V), HD 127423 (G0 V) and HD 128356 (K2.5 IV) obtained with the spectrograph HARPS at the ESO La Silla 3.6 m telescope in Chile. Our synthetic spectral fitting procedure was firstly verified by analysing the spectra of the Solar and Arcturus, which were used as a template stars with well-known abundances. Comparison of obtained synthetic and observed spectra allowed us to identify 98 spectral lines of 10 chemical elements (Si, Ca, Sc, Ti, V, Cr, Mn, Fe, Co, Ni) within wavelength range 4500Å < λ < 7000Å. Abundances of each chemical element in the atmospheres of three studied stars were determined using the equivalent width of identified lines.","PeriodicalId":52077,"journal":{"name":"Advances in Astronomy and Space Physics","volume":"1 1","pages":""},"PeriodicalIF":0.2000,"publicationDate":"2021-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":null,"platform":"Semanticscholar","paperid":null,"PeriodicalName":"Advances in Astronomy and Space Physics","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.17721/2227-1481.11.8-12","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"Q4","JCRName":"ASTRONOMY & ASTROPHYSICS","Score":null,"Total":0}
引用次数: 0
Abstract
We analysed spectra of HD 126535 (K1 V), HD 127423 (G0 V) and HD 128356 (K2.5 IV) obtained with the spectrograph HARPS at the ESO La Silla 3.6 m telescope in Chile. Our synthetic spectral fitting procedure was firstly verified by analysing the spectra of the Solar and Arcturus, which were used as a template stars with well-known abundances. Comparison of obtained synthetic and observed spectra allowed us to identify 98 spectral lines of 10 chemical elements (Si, Ca, Sc, Ti, V, Cr, Mn, Fe, Co, Ni) within wavelength range 4500Å < λ < 7000Å. Abundances of each chemical element in the atmospheres of three studied stars were determined using the equivalent width of identified lines.
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