{"title":"三颗恒星元素丰度的测定","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":"{\"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}","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
摘要
我们分析了HD 126535 (K1 V)， HD 127423 (G0 V)和HD 128356 (K2.5 IV)的光谱，这些光谱是由智利ESO La Silla 3.6 m望远镜上的HARPS光谱仪获得的。我们的合成光谱拟合程序首先通过分析太阳和大角星的光谱来验证，它们被用作已知丰度的模板星。将合成光谱与观测光谱进行比较，确定了波长范围4500Å < λ < 7000Å的10种化学元素(Si, Ca, Sc, Ti, V, Cr, Mn, Fe, Co, Ni)的98条谱线。三颗被研究的恒星大气中每种化学元素的丰度是用识别谱线的等效宽度来确定的。
On the determination of elemental abundances in three stars
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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