The two visible components of this system orbit each other over a period of 70.8 years with a large eccentricity of 0.63.[8] The primary component has a visual magnitude of 4.43, while the secondary is of magnitude 5.23.[3] Both are B-type main sequence stars with a stellar classification of B3 V.[5] One of the pair is itself a double-lined spectroscopic binary, making this a triple star system.[11]
^Houk, Nancy (1978), Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 2, Ann Arbor: Dept. of Astronomy, University of Michigan, Bibcode:1978mcts.book.....H.
^ abEdwards, T. W. (April 1976), "MK classification for visual binary components", Astronomical Journal, 81: 245–249, Bibcode:1976AJ.....81..245E, doi:10.1086/111879.
The system is listed in Table II as −44°9889.
^ abNitschelm, C. (December 2004), "Discovery and confirmation of some double-lined spectroscopic binaries in the Sco-Cen Complex", in Hilditch, R. W.; Hensberge, H.; Pavlovski, K. (eds.), In Spectroscopically and Spatially Resolving the Components of the Close Binary Stars, Proceedings of the Workshop held 20-24 October 2003 in Dubrovnik, Croatia, ASP Conference Series, vol. 318, San Francisco: Astronomical Society of the Pacific, pp. 291–293, Bibcode:2004ASPC..318..291N.