The two stars orbit each other with a period of only 2.15 days and aneccentricity of zero, indicating their orbit is close to circular.[6] They are orbiting sufficiently close to each other that their rotation periods have most likely becometidally locked—meaning they always maintain the same face toward each other.[9]
^abOja, T. (August 1991), "UBV photometry of stars whose positions are accurately known. VI",Astronomy and Astrophysics Supplement Series,89 (2):415–419,Bibcode:1991A&AS...89..415O
^abCowley, A.; et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications",Astronomical Journal,74:375–406,Bibcode:1969AJ.....74..375C,doi:10.1086/110819
^abOsawa, K.; Hata, S. (1962), "Three-color photometry of B8-A2 stars (II).",Annals of the Tokyo Astronomical Observatory,7: 209,Bibcode:1962AnTok...7..209O
^Wilson, R. E. (1953), "General Catalogue of Stellar Radial Velocities",Carnegie Institute Washington D.C. Publication, Carnegie Institute of Washington, D.C.,Bibcode:1953GCRV..C......0W
^abAbt, Helmut A.; Boonyarak, Chayan (November 2004), "Tidal Effects in Binaries of Various Periods",The Astrophysical Journal,616 (1):562–566,Bibcode:2004ApJ...616..562A,doi:10.1086/423795
