The distance to this star has been measured directly using the parallax method, yielding an estimated value of 43.96 light-years (13.48 parsecs).

[1] In 1976, this was reported as a spectroscopic binary system by Helmut A. Abt and Saul G. Levy, giving it an orbital period of 371 days.

[9] However, this was brought into question by Christopher L. Morbey and Roger F. Griffin in 1987, who suggested that the data could be explained by random chance.

[11] There is a 14th-magnitude common proper motion companion to Theta Ursae Majoris at an angular separation of 4.1 arcseconds,[12] so this may potentially be a triple star system.

[13] The primary component of this putative system has a published stellar classification of F6 IV,[3] indicating it is a subgiant star that is evolving away from the main sequence.