This is a double-lined spectroscopic binary system consisting of two near-identical, massive, O-type main sequence stars. Evolutionary tracks place the stars close to the zero age main sequence, with an age of less than two million years. This is a detached binary with a close orbit having a period of 2.11 days, and the orbit is assumed to have circularized. The orbital plane is estimated to be inclined by an angle of to the line of sight from the Earth, which yields mass estimates of 38 and 34 times the mass of the Sun. Although initially suspected to be an eclipsing binary and given a variable star designation, it doesn't appear to be eclipsing. Instead, the system displays ellipsoidal light variations that are caused by tidal distortions.
