论文标题
RW AUR B：著名初选的适度UX ORI类型同伴
RW Aur B: a modest UX Ori type companion of the famous primary
论文作者
论文摘要
著名的年轻二进制RW AUR的次要研究要少于初级。为了补偿这一缺点，我们在这里介绍了Rw Aur B的Ubvrijhk光度法，VRI极化和光谱观察结果，恒星在光带中表现出混乱的亮度变化，不规则短（〜1天）dimming lignied $ΔV$Δv$Δv$ 1.3^^。极化（在I频段中最多3％），大概是由于脉冲盘中尘埃散射的恒星辐射散射，这意味着可以将RW AUR B归类为UX ORI型恒星。我们得出的结论是，观察到的过剩排放量为$λ\ Lessim 0.45 $ $ $ $ m和longward $ \ $ \ $ \ $ 2 $μ$ m，以及HI，HEI和NAI D发射线的通量和轮廓的可变性，是由于增值过程所致。同时，Ca II线的发射成分表明RW AUR B具有强大的色层。 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.
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.
