The secondary component, 84 Ceti B, has a classification of K2V,[4] making it a K-type main sequence star. It lies at an angular separation of 3.3″ from the primary, which is equivalent to a physical separation of at least 74.5 AU.[4]
The space velocity components of this system are: –13(U), –25(V), –2(W) km/s.[8] Based upon the position and motion, it is a candidate member of the Tucana-Horologium Association; this is a group of stars that share a similar motion through space and hence may have originated in the same molecular cloud.[9] 84 Ceti is following an orbit through the Milky Way galaxy that has an eccentricity of 0.03, taking it as close as 22.3 kly (6.83 kpc) and as far as 26.2 kly (8.02 kpc) from the Galactic Center. The inclination of the orbital plane carries it as far as 260 ly (80 pc) away from the galactic plane.[8]
^ abcdRakos, K. D.; et al. (February 1982), "Photometric and astrometric observations of close visual binaries", Astronomy and Astrophysics Supplement Series, 47: 221–235, Bibcode:1982A&AS...47..221R.
^Nakajima, Tadashi; Morino, Jun-Ichi (January 2012), "Potential Members of Stellar Kinematic Groups within 30 pc of the Sun", The Astronomical Journal, 143 (1): 2, Bibcode:2012AJ....143....2N, doi:10.1088/0004-6256/143/1/2.