A Possible Explanation of W-type Phenomena in V694 Peg

Abstract

Three sets of complete multicolor light curves of V694 Peg observed in 2013, 2015, and 2019 were presented and analyzed. Our photometric solutions show that this system was an A-type shallow contact binary in 2013 and 2015 while it converted to a W-type one in 2019. A large cool spot on the component of this binary could explain the conversion, implying the W-type phenomena may be caused by the magnetic activity of the components. We have collected available data on this binary and calculated 505 times of light minimum, which spans 17 yr. The orbital period investigation based on these timings shows there is a long-term period increase at a rate of dP / dt = 4.3(±0.3)×10 ^−9 day yr ^−1 superposed on a periodic variation with a period of 11.81(±0.06) yr. The cyclic orbital variation may be the result of magnetic activity cycles or the existence of a third body. Until now, only eight transformed systems, including V694 Peg, have been reported. Compared with other converting contact systems between A-type and W-type, V694 Peg is recorded as the shortest-period one. All of these converting systems are late-type (later than F7) contact binaries with the O’Connell effect and show cyclic period variation, which indicates that magnetic activity may be the reason for the conversion between the two types of contact binaries. For investigating the nature of A-type and W-type phenomena, the discovery of more converting contact binaries is essential.

Keywords

• Close binary stars
• Contact binary stars
• Eclipsing binary stars
• Late-type stars
• Stellar evolution