Photometric Properties of the Variable Star LZ Herculis

We 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.