[en] In this paper, we present new CCD photometric observations of AH Tauri in the R band observed in 2006 at the Yunnan Observatory. Two new times of light minima were derived from these observations. We modeled the light curves using the 2003 version of the Wilson–Devinney program. The results show that the variations of the light curves can be expained by a cool spot on the primary star. The fill-out factor is about 6.6%, indicating that AH Tauri is a shallow-contact system. The mass ratio was determined to be about 0.505. In addition, the orbital period variations of AH Tauri were investigated based on all of the photoelectric and CCD light minimum times, including our two new data. It was found that the orbital period exhibits a possible periodic variation with a period of $P_{\mathrm{m}\mathrm{o}\mathrm{d}}=54.62(\pm <!--\; ??\; -->0.20)$ years and a secular period decrease of $dP/dt=-<!--\; ???\; -->(1.823\pm <!--\; ??\; -->0.215)\times <!--\; ??\; -->{10}^{-<!--\; ???\; -->7}\mathrm{d}\mathrm{a}\mathrm{y}\mathrm{s}{\mathrm{y}\mathrm{r}}^{-<!--\; ???\; -->1}$. Since AH Tauri is an overcontact solar-like system, we discuss three mechanisms of the mass transfer, the light-time effect of the third body, and magnetic activity responsible for the orbital period changes.