Binary Star System
This binary star system consists of two closely spaced low-mass red dwarf M-type stars. The secondary star is a dim magnitude 14 lost in the glare of the nearby primary star.
The most recent determination of the system orbital elements comes from a study by George Gatewood using older sources along with data from the Hipparcos satellite. This study yielded an orbital period of about 16.6 years and a semi-major axis separation of about 1.1 arc seconds.
Read more about this topic: Ross 614
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