It is visible to the naked eye as a faint, blue-white hued star with a baseline apparent visual magnitude of 5.18.

[5] From a twenty-year spectroscopic study, Hube and Aikman established a 367-day orbital period, and noted the presence of non-radial pulsations in the primary star.

Its photometric variation led to a variable star designation, as V377 Vulpeculae, but the non-reproducibility of the light curve made determination of the pulsation period elusive.

Continuous monitoring of the star by the Transiting Exoplanet Survey Satellite has revealed a beat-period phenomenon in the light curve, which causes the luminosity variations to fluctuate in amplitude.

[citation needed] The primary member, designated component A, is a most likely a B-type main-sequence star[7] with a stellar classification of B6 III.