BH Virginis

This system was determined to be a short period variable star by C. Hoffmeister in 1935. W. Zessewitsch found a period of 19.6 hours for the system in 1944. In 1957, M. Kitamura and associates refined the light curve of this Algol-type eclipsing variable and discovered some irregular fluctuations not explained by the eclipse cycle. R. H. Koch in 1967 reported observing a change in the depth of the primary eclipse. In 1982, M. Hoffmann concluded that both stars are intrinsically variable, indicating this is an RS Canum Venaticorum variable system.

This is a near-contact binary system with a circular orbit having a period of 19.61 hours. The orbital plane is inclined at an angle of 88° to the line of sight from the Earth, allowing both components to eclipse each other once per orbit. During the deep primary eclipse the system decreases in brightness by 0.96 magnitude, while the shallower secondary eclipse decreases the system by 0.64 magnitude. Cyclical oscillations in the orbital period have been observed with two short-term periods of 9.2 and 11.8 years, and a longer-term oscillation of 51.7 years. The short term oscillations may be due to magnetic activity on the stars, while the longer period could be caused by an unseen third body.

Both components of this system are G-type main-sequence stars, with stellar classifications of G0V and G2V, respectively. Evidence of star spots have been found on both stars, but appear to be predominantly on the secondary component. The two stars are somewhat larger and more massive than the Sun.