摘要：After an 11-year observing campaign, we present the combined visual–spectroscopic orbit of the formerly unremarkable bright star HR7345 (HD 181655, HIP 94981, GJ 754.2). Using the Separated Fringe Packet 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 three 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 HR7345 is observable for 15 days. Such a high eccentricity for HR7345 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±0.076Me and 0.926±0.075Me as well as an orbital parallax of 41.08±0.77 mas.
