论文标题
活性二进制原型RS Canum venaticorum的第一个多普勒成像
The first Doppler imaging of the active binary prototype RS Canum Venaticorum
论文作者
论文摘要
我们使用三种不同的望远镜和观测站点介绍了源自在2004年，2016年和2017年观察到的高分辨率光谱的原型活性二元星RS CVN的第一个多普勒图像。我们将最小二乘反向卷积的技术应用于所有观察到的光谱，以获得高信噪线轮廓，这些谱图用于推导活性K型组件的表面图像。我们的图像在K星上显示出复杂的斑点图案，在经度上广泛分布。我们的多普勒图像揭示的全星点位于约70 $^{\ circ} $的纬度下方。根据先前的光曲线建模研究，我们发现K星上没有一个极点。使用源自两个连续旋转循环的多普勒图像，我们估计表面差旋转速率为$ΔΩ= -0.039 \ pm 0.003〜RAD〜D^{ - 1} $和$α=δΩ/ω_________________________________________________________________________________________________{eq} = -0.030 \ pm 0.002 \ for k Star for K Star。鉴于这两个旋转期间的相位覆盖率有限，因此我们的差异旋转估计值的不确定性大概更高。
We present the first Doppler images of the prototypical active binary star RS CVn, derived from high-resolution spectra observed in 2004, 2016 and 2017, using three different telescopes and observing sites. We apply the least-squares deconvolution technique to all observed spectra to obtain high signal-to-noise line profiles, which are used to derive the surface images of the active K-type component. Our images show a complex spot pattern on the K star, distributed widely in longitude. All starspots revealed by our Doppler images are located below a latitude of about 70$^{\circ}$. In accordance with previous light-curve modeling studies, we find no indication of a polar spot on the K star. Using Doppler images derived from two consecutive rotational cycles, we estimate a surface differential rotation rate of $ΔΩ= -0.039 \pm 0.003 ~rad~d^{-1}$ and $α= ΔΩ/Ω_{eq} = -0.030 \pm 0.002$ for the K star. Given the limited phase coverage during those two rotations, the uncertainty of our differential rotation estimate is presumably higher.
