Based on its parallax, it is located some 1,490 light-years away,[2] and it has an apparent magnitude of about 5.2, making it visible to the naked eye.

[8] Although the secondary has an effective temperature of nearly 12,000 K and the primary just 4,700 K, the large size of the cooler star means it is nearly 20 times as luminous at 2,200 L☉.

The eclipses are deeper at shorter wavelengths because a greater proportion of the short-wavelength radiation comes from the hot star.

The primary eclipses last for eight days at visual wavelengths, but partial phases can be detected for up to 17 days at ultraviolet wavelengths due to the expanded atmosphere and wind of the primary star.

Secondary eclipse, where the hot star transits the cooler one, are undetectable, and ellipsoidal variations due to distortion of the large primary produce brightness changes of less than 1.5%.