VV Corvi

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VV Corvi (abbreviated as VV Crv) is an eclipsing binary in the constellation Corvus. At an apparent magnitude of 5.843, the system is faintly visible to the naked eye in regions not significantly affected by light pollution. Parallax measurements imply a distance of 266 light-years (82 parsecs). The two stars orbit each other with an orbital period of 1.46 days and an eccentricity of 0.088. The primary is 1.98 times as massive as the Sun, has 3.375 the Sun's radius and 18 its luminosity. The secondary is 1.513 times as massive as the Sun, has 1.650 the Sun's radius and 4.745 times its luminosity. Both are F-type main-sequence stars of spectral type F5V, though the primary has begun expanding and cooling as it nears the end of its time on the main sequence. A tertiary companion was discovered during the Two Micron All-Sky Survey. VV Corvi makes part of a multiple star system. It is the secondary component of the sextuple star system ADS 8627, whose primary member is HR 4822, a magnitude 5.98 star separated by 5.24" from VV Corvi, which at the system's distance implies a projected separation of 416 astronomical units and an orbital period around 3,500 years. HR 4822 is itself a triple star system. The third component, separated by 59.5" from the primary and secondary, is BD-12°3675, a magnitude 10.28 star.