The distance to this star is approximately 460 light years based on parallax measurements.

[10] In 1965, W. P. Bidelman discovered that the intensities of the star's neutral helium lines had varied on photographic plates taken over the period 1908 to 1911.

[12] This is a magnetic peculiar Bp star that shows periodic variation in the strength of its neutral helium lines.

It is classified as an SX Arietis type variable star and its brightness varies from magnitude +4.38 to +4.43 with a period of 8.82 days.

[8] The variation in helium concentration effects the density scale height of the atmosphere, causing helium rich regions to have a lower luminosity in the visual band but emitting stronger levels of far ultraviolet.