Photometric Properties of the Variable Star LZ Herculis

Abstract

ABSTRACTWe present BV photometric results of the variable star LZ Her. Frolov & Irkaev classified it as a field SX Phe–type pulsating star, but our observations clearly show that LZ Her is not an SX Phe star, but rather a W UMa–type eclipsing binary, as reported by Garrido et al. The orbital period is derived to be 0.33173646 days by combining our data with that in the literature. The eclipsing light‐curve solution from the Wilson‐Devinney code shows that LZ Her belongs to the W subgroup of W UMa stars; the primary component is less massive and hotter, with a spectral type of F9–G0, and the secondary is more massive and cooler, with a spectral type G5–G6. The spectral types were estimated from the photometric light‐curve solution. Asymmetric light curves could be explained by assuming a cool spot on the secondary star. In the observing field of LZ Her, we found a new eclipsing binary, 2MASS 17500367+2928020, with an orbital period of 0.3056 days.