This system is visible to the naked eye as a faint blue-white hued star with a maximum apparent visual magnitude of +5.587.

[8] The binary nature of the brighter component was discovered in 1910 by astronomer Oliver J. Lee at Yerkes Observatory.

The first orbital elements were published by Otto Struve and Nicholay T. Bobrovnikov in 1925.

[12] This is a single-lined spectroscopic binary with an orbital period of 12.1 days and a small eccentricity of 0.05.

This component is a Beta Cephei variable star with three dominant pulsation modes having frequencies of around six per day.