Gamma Circini is a star system in the constellation Circinus. Its name is a Bayer designation that is Latinized from γ Circini, and abbreviated Gamma Cir or γ Cir. This was noted as a double star by Herschel in 1835, who estimated the separation as 1 arc second. It is visible to the naked eye as a point of light with a combined apparent visual magnitude of 4.51. Based upon an annual parallax shift of , it is about 450 light-years away.
This is a wide binary star system and may even be a triple star. The two visible components orbit each other with a preliminary estimated period of 258 years and a large eccentricity of 0.931. As of 2014, the visible components have an angular separation of 0.80 arc seconds on a position angle of 359°.
The primary star, component A, is a B-type subgiant star with a stellar classification of B5 IV. Based upon isochrone curve fitting it is hypothesized to be a pair of matching B5 stars, and is a Be variable with an uncertain maximum. It has an effective temperature of 15,135 K and an estimated mass six times that of the Sun. The companion, component B, is an F-type main-sequence star with a stellar classification of F8 V. It has an effective temperature of 4,786 K.
References
External links http://server3.wikisky.org/starview?object_type=1&object_id=1111