УДК 53 Физика
УДК 520 Инструменты, приборы и методы астрономических наблюдений, измерений и анализа
УДК 521 Теоретическая астрономия. Небесная механика. Фундаментальная астрономия. Теория динамической и позиционной астрономии
УДК 523 Солнечная система
УДК 524 Звезды и звездные системы. Вселенная Солнце и Солнечная система
УДК 52-1 Метод изучения
УДК 52-6 Излучение и связанные с ним процессы
ГРНТИ 41.00 АСТРОНОМИЯ
ГРНТИ 29.35 Радиофизика. Физические основы электроники
ГРНТИ 29.31 Оптика
ГРНТИ 29.33 Лазерная физика
ГРНТИ 29.27 Физика плазмы
ГРНТИ 29.05 Физика элементарных частиц. Теория полей. Физика высоких энергий
ОКСО 03.06.01 Физика и астрономия
ОКСО 03.05.01 Астрономия
ОКСО 03.04.03 Радиофизика
ББК 2 ЕСТЕСТВЕННЫЕ НАУКИ
ББК 223 Физика
ТБК 614 Астрономия
ТБК 6135 Оптика
BISAC SCI004000 Astronomy
BISAC SCI005000 Physics / Astrophysics
We present the study of the He-weak star HD 188101. Using spectral observations obtained with the Main stellar spectrograph (MSS) and the Nasmyth echelle spectrograph (NES) mounted on the BTA SAO RAS and the data from the literature, we determined the fundamental parameters: $T_{\rm eff}=15600 \pm 400$ K, $\log g_{\rm spec} = 3.87 \pm 0.13$, $R = 2.1-3.1$ $R_{\odot}$, $M = 3.8-4.8$ $M_{\odot}$. Chemical abundances were determined by the synthetic spectrum method: under the LTE assumption for He, N, Ti, Fe and without LTE for C, O, Mg, Si. For Si and Fe, overabundance of about 0.6 dex relative to the solar abundance was found. The non-LTE calculations with the stellar Si abundance lead to consistent abundances from lines of Si II and Si III, while the difference between LTE abundances amounts to 0.8 dex.
stars: chemically peculiar, abundances, atmospheres, magnetic fields
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