[1] In 1903, the luminosity of this system was found to vary by the German astronomers Gustav Müller and Paul Kempf.

[10] This system consists of a pair of stars in a tight, circular orbit with a period of 0.3336 days, or eight hours and 26 seconds.

As a result, they have the same stellar classification of F8Vp, which matches the spectrum of a main-sequence star that is generating energy through the nuclear fusion of hydrogen.

[5] The orbital period of the system has changed since 1903, which may be the result of mass transfer or the braking effects of magnetic fields.

[10] W Ursae Majoris has a 12th magnitude companion star with the designation ADS 7494B, not to be confused with W UMa B, the secondary of the close eclipsing pair.