W Большой Медведицы
VV Corvi is a close spectroscopic binary, its two component stars orbiting each other with a period of 1.46 days. Both are yellow-white 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. The mass ratio of the two stars is 0.775 ± 0.024. A tertiary companion was discovered during the Two Micron All-Sky Survey. W Corvi is an eclipsing binary that varies in brightness from apparent magnitude 11.16 to 12.5 over 9 hours. Its period has increased by 1/4 second over a century. It is an unusual system in that its two stars are very close to each other yet have different surface temperatures, and hence thermal transfer is not taking place as expected. SX Corvi is an eclipsing binary that is also a contact binary known as a W Ursae Majoris variable. The two component stars orbit closely enough to each other for mass to have been transferred between them—in this case the secondary having transferred a large amount of mass to the primary. RV Corvi is another eclipsing binary. Its brightness varies from apparent magnitude 8.6 to 9.16 over 18 hours. The system is composed of stars of spectral types F0 and G0, which orbit each other every 0.7473 days.