Atmospheric iron abundance in the primary component of υ Sgr |
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Authors: | V V Leushin |
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Institution: | (1) Special Astrophysical Observatory, Russian Academy of Sciences, Nizhnii Arkhyz, Stavropolskii Krai, 357147, Russia |
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Abstract: | Based on the observed energy distribution and line spectrum of the primary component of the binary υ Sgr, we computed blanketed model atmospheres. The atmospheric iron abundance in the primary component of υ Sgr was derived from photographic and CCD spectra. Our analysis confirmed the previously inferred T eff = 13500 ± 150 K and logg = 2.0 ± 0.5. The microturbulent velocity was found from spectral lines in different spectral ranges to be V t = 8–12 km s?1. We refined the mass fractions of light elements: 10?4 for H, 0.91 for He, 0.013 for C, 0.049 for N, and 0.008 for O. The iron abundance was determined with a high accuracy from Fe I, Fe II, and Fe III lines in the spectral range 4000–7000 Å: log (N(Fe)/∑N i ) = ?3.80±0.20. |
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Keywords: | stars-variable and peculiar |
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