This is a double-linedspectroscopic binary star system with an orbital period of 31.39 days and aneccentricity of 0.53.[6] The members are separated by a distance of0.33 AU. The primary and secondary components havestellar classifications of A8III and A3III respectively, indicating that theyevolved away from themain sequence and are nowgiant stars. Component A is 2.6 times more massive than the Sun, but expanded to 4.4 the Sun's radius[a] and irradiates 60 times more than the Sun. Component B is somewhat smaller and less luminous, being 2.25 times more massive, 2.44 times larger[b] and 30 times brighter than the Sun. The system has an age around 400 million years, less than 10% that of theSolar System.[3] Beta Trianguli is among the leastvariable of the stars that were observed by theHipparcos spacecraft, with a magnitude varying by only 0.0005.[12]
Based on observations using theSpitzer Space Telescope, as reported in 2005, this system is emitting anexcess of infrared radiation. This emission can be explained by a circumbinaryring of dust. The dust is emitting infrared radiation at a blackbody temperature of 100 K.[13] It is thought to extend from 50 to 400 AU away from the stars.[14]
^abcJohnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars",Communications of the Lunar and Planetary Laboratory,4 (99): 99,Bibcode:1966CoLPL...4...99J
^Gray, R. O.; Corbally, C. J.; Garrison, R. F.; McFadden, M. T.; Robinson, P. E. (2003). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 Parsecs: The Northern Sample. I".The Astronomical Journal.126 (4): 2048.arXiv:astro-ph/0308182.Bibcode:2003AJ....126.2048G.doi:10.1086/378365.S2CID119417105.
^Stansberry, J. A.; et al. (2005). "A Spitzer Survey for Debris Disks in Binary Star Systems".Protostars and Planets V, Proceedings of the Conference held October 24-28, 2005, in Hilton Waikoloa Village, Hawai'i. p. 8613.Bibcode:2005prpl.conf.8613S.
