The system is barely visible to the naked eye in good seeing conditions, having a peak apparent visual magnitude of 5.91.

[5] This is a double-lined spectroscopic binary in a close, circular orbit with a period of 10.08 days and a separation of 40.327 R☉ (28.055 Gm).

[1] Samus et al. (2017) classify this as a detached Beta Lyrae-type eclipsing binary, although they note there is some uncertainty in the classification.

[3] Bossi et al. (1998) argued that the system is neither an eclipsing binary nor an ellipsoidal variable.

[9] Linnell et al. (2006) demonstrated that the light curve is mostly caused by tidal distortion in combination with illumination of the lower mass secondary by the primary.