59 Serpentis appears as a close pair of stars, of 5th magnitude and 7th magnitude respectively, separated by four arc-seconds. The brighter of the two is itself an even closer binary with the two stars separated by only 0.2″, and only 0.1″ when they were first detected. The stars are designated Aa, Ab, and B.[12]
The primary star, component Aa, is a G0 giant. Component Ab is spectroscopic binary with a period of 1.85 days; the two stars are very similar A-class main sequence stars. Component B is an F5V possible astrometric binary, but with little known about the orbit or the possible companion.[8]
A much fainter star 20″ away is also thought to be a member of the system, having a common proper motion and similar Gaia parallax, and is designated as component C.[8]
^ abMermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode:1986EgUBV........0M.
^Wilson, Ralph Elmer (1953). "General catalogue of stellar radial velocities". Carnegie Institute Washington D.C. Publication. Bibcode:1953GCRV..C......0W.