New CCD observations for V802 Aql were observed from 2004 to 2007, and seven light minimum timings were obtained. Using the Wilson-Devinney code, the photometric solution was deduced from R-band observations. The results show that the mass-ratio and the contact degree are q = 0.1443 ± 0.0059 and f = 34.9% ± 7.6%, respectively. Comparing the parameters of the dark spot from our results with those from Samec et al., it is found that the magnetic activity of the primary component may have been migrating towards its equator from 2002 to 2005. An orbital period analysis weakly suggests that the orbital period may undergo a cyclic variation with a period of P3 = 8.32yr and an amplitude of A = 0.d0196. The periodic oscillation of this binary may be more plausibly explained as being the result of magnetic activity cycles. Therefore, the eclipsing star V802 Aql may be coalescing via magnetic breaking. © 2008. Astronomical Society of Japan.