The T Tauri spectroscopic binary GW Orionis
The T Tauri spectroscopic binary GW Orionis
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金牛座 T 光谱双星猎户座 GW
DOI：
10.1086/115841
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发表时间：
1991
期刊：
影响因子：
--
通讯作者：
D. Latham
中科院分区：
文献类型：
--
作者：
R. Mathieu;F. Adams;D. Latham
经典的金牛座 T 星 GW Ori 被发现是一颗光谱双星，其轨道周期为 242 天。给出的径向速度数据表明 GW Ori 是一个速度变量，列出了光谱轨道元素，并给出了不同倾角下二次和一次/二次分离的动态质量。基于具有强硅酸盐发射的双峰双峰通量分布，详细考虑了光谱能量分布的两个理论模型。纯盘模型由主星、环主星盘和环双星盘以及盘之间光学上薄的热尘埃组成，除了 13-18 微米范围内的较高光度外，被发现符合光谱分布。还考虑了盘壳模型，其中光学薄壳取代了环绕双星盘。尽管视觉消光必须大于观测到的 A(v)，但该模型很好地拟合了光谱分布。考虑双星圆形轨道理论的重要性，特别注意双星轨道中圆盘引起的偏心率激发。 53 参考文献
The classical T Tauri star GW Ori is found to be a spectroscopic binary whose orbital period is 242 days. Radial velocity data are presented which show that GW Ori is a velocity variable, the spectroscopic orbital elements are listed, and the dynamic masses for secondary and primary/secondary separations at different inclination angles are given. Two theoretical models for the spectral energy distribution are considered in detail, based on the binary's flux distribution which is double peaked with a strong silicate emission. The pure-disk model, consisting of a primary star, both a circumprimary and circumbinary disk, and optically thin hot dust between the disks, is found to fit the spectral distribution with the exception of higher luminosity in the 13-18 micron range. A disk-shell model is also considered in which an optically thin shell replaces the circumbinary disk. This model fits the spectral distribution well although the visual extinction must be larger than the observed A(v). The significance of the circular orbit theorized for the binary is considered with special attention given to the disk-induced excitation of eccentricity in binary orbits. 53 refs.