We present spectroscopic observations of LX Per carried out using the Korean Bohyunsan Observatory Echelle Spectrograph (BOES) with spectral resolving power R = 80, 000. The spectrograph was attached to the 1.8?m telescope. The fit of synthetic spectra to the observed spectrum of the system allowed us to find the component parameters and the abundances of chemical elements in the atmospheres of the components. The strong Ca II H&K emissions are confirmed; we also found emission lines in the Ca II reversals' triplet absorptions at the wavelengths of 8498, 8542, and 8662?? in the spectrum of the cooler component of LX Per. A unique photometric solution using the distorted light curves of three different epochs was made. The spot model light curves were fitted to the 1981, 1982, and 1983 observations successfully by adjusting only spot parameters. We could infer that the variation of spot location and size was the main reason for the changing shape of light curves. The main feature of the abundance patterns of both components was the apparent deficiency of heavy (Z 30) elements. Only elements with strong lines, namely Y and Ba, were detected. Correlations of relative abundances of chemical elements with condensation temperatures and second ionization potentials of these elements, which can be explained by the accretion of dust and gas, were found.
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机译：我们目前使用韩国Bohyunsan天文台埃歇尔光谱仪（BOES）进行的LX Per光谱观察，光谱分辨力R = 80，000。该光谱仪安装在1.8？m望远镜上。合成光谱与系统观测光谱的拟合使我们能够找到组分参数以及组分大气中化学元素的丰度。证实了Ca II H＆K的强烈排放;我们还发现了Ca II逆转的三重态吸收在8498、8542和8662波长处的发射谱线？在LX Per。使用三个不同历元的扭曲光曲线，制作了一个独特的光度学解决方案。通过仅调整点参数，将点模型的光曲线成功地拟合到1981、1982和1983的观测值。我们可以推断出光斑位置和大小的变化是光曲线形状变化的主要原因。两种成分的丰度模式的主要特征是明显缺乏重元素（Z> 30）。仅检测到具有强线的元素，即Y和Ba。发现了化学元素的相对丰度与冷凝温度和这些元素的第二电离势的关系，这可以通过灰尘和气体的积聚来解释。
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