Based upon parallax measurements made during the Hipparcos mission, this star system is located at a distance of roughly 437 light-years (134 parsecs) from Earth.

[1] This is a single-lined spectroscopic binary system, which means that the two stellar components have not been individually resolved with a telescope.

The gravitational perturbation of the hidden secondary component upon the primary is causing the latter to first move toward and then away from the Earth, creating Doppler shift changes in the spectrum.

[7] The interaction between the two components of this system appears to be creating emission lines in the spectrum, turning the primary into a Be star.

It is a Beta Cephei type variable star with a brightness that periodically varies from magnitude +3.38 to +3.41 over an interval of 0.17 days.