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Star in the constellation Andromeda
This article is about the star. For the galaxy, see Andromeda IX.
This system was determined to be a single-lined spectroscopic binary in 1916 by American astronomer W. S. Adams, and the initial orbital elements were computed by Canadian astronomer R. K. Young in 1920. The pair orbit each other with a period of 3.2196 days and an eccentricity of 0.03. It is an eclipsing binary, which means the orbital plane is inclined close to the line of sight and, from the perspective of the Earth, the stars pass in front of each other, causing two partial eclipses every orbit. During the transit of the secondary in front of the primary, the visual magnitude drops to 6.16, while the eclipse of the secondary by the primary lowers the net magnitude to 6.09.
Hill, G.; et al. (1975), "MK Classifications of some Northern Hemisphere Binary Systems", Memoirs of the Royal Astronomical Society, 79: 131, Bibcode:1975MmRAS..79..131H.
^ Tremko, Jozef; Bakos, Gustav A. (October 1978), "A Photometric Study of the Am Binary System AN Andromedae", Journal of the Royal Astronomical Society of Canada, 72: 263, Bibcode:1978JRASC..72..263T.