HR 7578 - A K dwarf double-lined spectroscopic binary with peculiar abundances
HR 7578 - A K dwarf double-lined spectroscopic binary with peculiar abundances
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HR 7578 - 具有特殊丰度的 K 矮星双线光谱双星
DOI：
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发表时间：
1983
期刊：
影响因子：
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通讯作者：
W. Beavers
中科院分区：
文献类型：
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作者：
F. Fekel;W. Beavers
目前已知的双线K型和M型矮双星的数量相当少，每种类型只有十几颗或更少。HR 7578系统在威尔逊山系统上被归类为dK5，在MK E1系统上被归类为K2 V。表中列出了径向速度测量的摘要，包括观测站和每次观测的重量。具有较强谱线的星星被称为分量A。用Barker等人（1967年）描述的微分修正计算机程序计算出所有观测值适当加权后的最终轨道根数解。该程序已被修改为双线的情况。特别令人感兴趣的是非常大的偏心率的系统和大的最小质量为每个组件。这些巨大的最小质量表明，尽管恒星的周期相对较长，半径较小，但日食还是可以被探测到的。
The number of double-lined K and M dwarf binaries which is currently known is quite small, only a dozen or less of each type. The HR 7578 system was classified as dK5 on the Mount Wilson system and as K2 V on the MK ystem. A summary of radial-velocity measurements including the observatory and weight of each observation is given in a table. The star with the stronger lines has been called component A. The final orbital element solution with all observations appropriately weighted was computed with a differential corrections computer program described by Barker et al. (1967). The program had been modified for the double-lined case. Of particular interest are the very large eccentricity of the system and the large minimum masses for each component. These large minimum masses suggest that eclipses may be detectable despite the relatively long period and small radii of the stars.