使用CHARA阵列III进行的分离条纹数据包观测。超高偏心双星HR 7345
Separated Fringe Packet Observations with the CHARA Array III. The Very High Eccentricity Binary HR 7345
摘要：
经过十一年的观测活动，我们给出了以前不起眼的亮星HR 7345（HD 181655、HIP 94981、GJ 754.2）的组合视光谱轨道。使用分离边缘包（SFP）方法和CHARA阵列，我们能够确定一个难以完成的轨道周期为331.609 +/- 0.004天。这11个月的周期使得该系统在干涉仪观测中被隐藏在太阳后面，每次隐藏3年。由于轨道的高偏心率约为一年的90%，在2018年1月之后，近星点阶段将无法再次观测到，直到2021年底。由于其极高的偏心率（0.9322 +/- 0.0001），HR 7345的双线光谱相位可以观测15天。HR 7345如此高的偏心率使其成为可见和光谱轨道目录中最偏心的系统之一。对于这个系统，我们确定几乎相同的组件质量为0.941 +/- 0.076 Msun和0.926 +/- 0.075 Msun以及41.08 +/- 0.77 mas的轨道视差。
英文摘要：
After an eleven year observing campaign, we present the combined visual{spectroscopic orbit of the formerly unremarkable bright star HR 7345 (HD 181655, HIP 94981, GJ 754.2). Using the Separated Fringe Packet (SFP) method with the CHARA Array, we were able to determine a difficult to complete orbital period of 331.609 +/- 0.004 days. The 11 month period causes the system to be hidden from interferometric view behind the Sun for 3 years at a time. Due to the high eccentricity orbit of about 90% of a year, after 2018 January the periastron phase will not be observable again until late 2021. Hindered by its extremely high eccentricity of 0.9322 +/- 0.0001, the double-lined spectroscopic phase of HR 7345 is observable for 15 days. Such a high eccentricity for HR 7345 places it among the most eccentric systems in catalogs of both visual and spectroscopic orbits. For this system we determine nearly identical component masses of 0.941 +/- 0.076 Msun and 0.926 +/- 0.075 Msun as well as an orbital parallax of 41.08 +/- 0.77 mas.
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