The two stars orbit each other with an orbital period of 1.46 days and an eccentricity of 0.088.[7] 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.[4] A tertiary companion was discovered during the Two Micron All-Sky Survey.[8]
VV Corvi makes part of a multiple star system. It is the secondary component of the sextuple[a] star system ADS 8627, whose primary member is HR 4822,[4] a magnitude 5.98 star separated by 5.24" from VV Corvi,[9] which at the system's distance implies a projected separation of 416 astronomical units and an orbital period around 3,500 years.[4] HR 4822 is itself a triple star system.[4] The third component, separated by 59.5" from the primary and secondary, is BD-12°3675, a magnitude magnitude 10.28 star.[9]
Notes
^While classified as a quintuple in Fekel et al. 2013, with BD-12°3675 being only a candidate member, BD-12°3675 was included in Tokovinin's Multiple Star Catalog.[9]
^ abJohnson, H. L.; Iriarte, B.; Mitchell, R. I.; Wisniewskj, W. Z. (1966). "UBVRIJKL photometry of the bright stars". Communications of the Lunar and Planetary Lab. 4 (3): 99. Bibcode:1966CoLPL...4...99J.
^Batten, A. H. (1967). "Sixth catalogue of the orbital elements of spectroscopic binary systems". Publications of the Dominion Astrophysical Observatory, Victoria. 13: 119–251. Bibcode:1967PDAO...13..119B.
