SIMBAD references

The U, B and V observations confirmed, once more, after Vetesnik & Perek (1965, BAC 42, 119) that CV Cygni is an eclipsing binary of W UMa type. Due to the variable depth (up to 0.1 magnitude) of one of the minima, the system shifts from A to W-type (or vice versa). The (O-C) diagram of all available times of minima confirms the continous period decrease with a rate dP/dt≃4.44x10^–7day/yr. The relatively large orbital period (P≃0.98day), the shape of the light and color curves, and the position of the system in the color-period diagram indicate that CV Cyg is an interesting highly evolved contact or near-contact binary which is rapidly evolving into deeper contact through the angular momentum loss from the system.