The inner pair is orbited by the 9.4 magnitude B component, at anangular separation of 7.1 arcseconds. A fourth component C, 69.6 arcseconds away, has an apparent magnitude of 10.4.[3] However, component C is an optical companion: it is physically unrelated and only appears close in the sky.[10]
On 11 November 2028 and again 11 November 2036, it will have close conjunctions withVenus.[13]: 167
^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.
^abcdeRomanovskaya, A M; Ryabchikova, T A; Pakhomov, Yu V; Korotin, S A; Sitnova, T M (2023-12-11), "Non-LTE abundance analysis of A-B stars with low rotational velocities – II. Do A-B stars with normal abundances exist?",Monthly Notices of the Royal Astronomical Society,526 (3):3386–3399,arXiv:2309.08384,doi:10.1093/mnras/stad2862,ISSN0035-8711.
^Adelman, Saul J. (November 1997), "On the possible variability of the main sequence A stars theta Virginis and 109 Virginis",Astronomy & Astrophysics Supplement Series,125 (3):497–499,Bibcode:1997A&AS..125..497A,doi:10.1051/aas:1997105.
^Scholz, G.; et al. (September 1998), "Spectroscopic and photometric investigations of MAIA candidate stars",Astronomy and Astrophysics,337:447–459,Bibcode:1998A&A...337..447S.
