Components A and B of this system form a wide binary.[13] The secondary, component B, is a magnitude 10.7 stellar companion at an angular separation of 9.29″ from the primary along a position angle of 35.72°, as of 2009. The primary was identified as a spectroscopic binary by E. B. Frost in 1924.[14] This companion was confirmed during a lunar occultation with a separation of 14.1±0.7 mas and magnitude 6.8.[15]
This star is less than a billion years in age with a rapid spin, showing a projected rotational velocity of 154 km/s[9] It is larger and hotter than the Sun, with twice the Sun's mass and 2.8 times the radius of the Sun. The star is radiating 27 times the Sun's luminosity from its photosphere at an effective temperature of 7,932 K.[3]
The primary displays a significant infrared excess in the K-band, which indicates an orbiting circumstellar disk of dust. A model fit to the data shows an inner radius between 0.08 AU and 0.14 AU, and an outer radius of up to 0.65 AU.[10]
^ abcdGutierrez-Moreno, Adelina; et al. (1966), "A System of photometric standards", Publications of the Department of Astronomy University of Chile, 1, Publicaciones Universidad de Chile, Department de Astronomy: 1–17, Bibcode:1966PDAUC...1....1G.
^Richichi, A.; et al. (October 1999), "New binary stars discovered by lunar occultations. IV", Astronomy and Astrophysics, 350: 491−496, Bibcode:1999A&A...350..491R.
