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arXiv 2007.12559astro-ph.SR
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RW Aur B：著名的主天体的一个普通的UX Ori型伴星

RW Aur B: a modest UX Ori type companion of the famous primary

A. Dodin, S. Lamzin, P. Petrov, B. Safonov, M. Takami, A. Tatarnikov

备注：
12 pages, accepted by MNRAS
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摘要：

著名的年轻双星RW Aur的次级星比初级星的研究要少得多。为了弥补这一不足，本文给出了对RW Aur B的UBVRIJHK测光、VRI偏振和光谱观测结果。这颗恒星在光学波段表现出混乱的亮度变化，不规则的短（~ 1天）变暗，幅度$ΔV$高达$1.3^{\rm m}.$变暗伴随着线性偏振的增加（在I波段高达3%），这可能是由于星周盘中的尘埃散射了恒星辐射，这意味着RW Aur B可以被归类为UX Ori型恒星。我们的结论是，观测到的过量发射在$λ\lesssim 0.45$ $μ$ m和longward $\approx$ 2 $μ$ m以及变化的流量和配置文件的HI，HeI和NaI D发射线是由于吸积过程。同时，Ca II线的发射分量表明RW Aur B具有强大的色球。假设太阳元素丰度，我们发现了以下参数的恒星：$T_{\rm eff} = 4100-4200$ K，$A_{\rm V}=0.6 \pm 0.1$（出的调光事件），$L_* \approx 0.6$ $L_\odot,$ $R_* \approx 1.5$ $R_\odot,$ $M\approx 0.85$ M $_\odot,$ $\dot M_{\rm acc}<5\times 10^{-9}$ M $_\odot$年$^{-1}.$最后，我们讨论了可能的原因不同水平的吸积活动的RW Aur二进制组件和目前的论点赞成的事实，它们是引力约束。

英文摘要：

The secondary of the famous young binary RW Aur is much less studied than the primary. To compensate this shortcoming, we present here the results of UBVRIJHK photometric, VRI polarimetric and optical spectral observations of RW Aur B. The star demonstrates chaotic brightness variations in the optical band with irregular short (~ 1 day) dimmings with an amplitude $ΔV$ up to $1.3^{\rm m}.$ The dimmings are accompanied with an increase in the linear polarization (up to 3 per cent in the I band), presumably due to the scattering of the stellar radiation by dust in the circumstellar disc that means that RW Aur B can be classified as a UX Ori type star. We concluded that the observed excess emission at $λ\lesssim 0.45$ $μ$m and longward $\approx$ 2 $μ$m as well as a variability of fluxes and profiles of HI, HeI and NaI D emission lines are due to the accretion process. At the same time, emission components of Ca II lines indicate that RW Aur B has a powerful chromosphere. Assuming the solar elemental abundances, we found the following parameters of the star: $T_{\rm eff} = 4100-4200$ K, $A_{\rm V}=0.6 \pm 0.1$ (out of the dimming events), $L_* \approx 0.6$ $L_\odot,$ $R_* \approx 1.5$ $R_\odot,$ $M\approx 0.85$ M$_\odot,$ $\dot M_{\rm acc}<5\times 10^{-9}$ M$_\odot$ yr$^{-1}.$ Finally, we discuss possible reasons for the different levels of the accretion activity of RW Aur binary components and present arguments in favour of the fact that they are gravitationally bound.

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