omega draconis is a spectroscopic binary, which means the two stellar components are too close to be resolved but periodic doppler shifts in their spectra indicate orbital motion. in this case, light from both stars can be detected, and it is a double-lined spectroscopic binary. the orbital period of the system is 5.28 days, and the eccentricity of the system is 0.00220, implying a nearly circular orbit. the primary has a mass of , and is an f-type main-sequence star. the secondary is less massive, at .