R. M. Bayazitov, L. I. Mashonkina, Yu. V. Pakhomov, I. A. Yakunin
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引用次数: 0
Abstract
Based on spectroscopic and photometric observations, we have determined the fundamental parameters of the poorly studied star HD 188101 with a weak magnetic field. Its effective temperature \(T_{\textrm{eff}}=14\,200\pm 990\) K and surface gravity \(\log g=3.70\pm 0.16\) are typical for main-sequence B9 stars. The He, C, O, Mg, Si, Ti, and Sr abundances have been determined by taking into account the departures from local thermodynamic equilibrium. Overabundances of Si, Ti, and Sr relative to their solar abundances have been revealed. The He abundance is lower than the solar one, but the difference is within the error limits. In addition to the photometric variability known from Kepler data, we have found changes in absorption for He I, Mg II, Si II, Si III, Ti II, and Fe II lines, with different He I and Mg II lines giving different abundances for the same phase of observations. The star HD 188101 is shown to belong to the group of chemically peculiar He-weak SiTiSr stars.
基于光谱和光度观测，我们确定了在弱磁场下研究较少的恒星HD 188101的基本参数。它的有效温度\(T_{\textrm{eff}}=14\,200\pm 990\) K和表面重力\(\log g=3.70\pm 0.16\)是典型的主序B9恒星。He， C， O, Mg, Si， Ti和Sr丰度的确定考虑了局部热力学平衡的偏离。硅、钛和锶相对于它们的太阳丰度的过丰度已经被揭示。氦丰度低于太阳丰度，但差异在误差范围内。除了开普勒数据中已知的光度变化外，我们还发现了He I， Mg II, Si II, Si III， Ti II和Fe II谱线的吸收变化，不同的He I和Mg II谱线在同一观测阶段给出了不同的丰度。恒星HD 188101被证明属于化学上特殊的he弱SiTiSr恒星群。
期刊介绍：
Astronomy Letters is an international peer reviewed journal that publishes the results of original research on all aspects of modern astronomy and astrophysics including high energy astrophysics, cosmology, space astronomy, theoretical astrophysics, radio astronomy, extragalactic astronomy, stellar astronomy, and investigation of the Solar system.
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