The two components are almost identical pre-main-sequence stars in a close circular orbit, and they show shallow eclipses that produce brightness variations of a few tenths of a magnitude.

Each component of the binary system is slightly under 3 M☉.

Although they have a subgiant spectral classification, they are still contracting onto the main sequence and are estimated to be only about 500,000 years old.

[8] It is estimated that they will reach the main sequence as smaller hotter late-B stars.

[7] The variability was first reported in 1954[2] and confirmed as an eclipsing binary in 2012.