CCD, BVRI light curves of V1302 Her were taken on 24, May, 07, and 23. 24, 27 June 2020 at the Dark Sky Observatory, North Carolina with the 32-inch reflector of Appalachian State University. The variability of V1302 Her (GSC 3101-0683) was discovered in the FOV of V338 Her by the ROTSE1 experiment (Akerlof 2000). Liakos (2009) reported a new period of Min. I = 2454610.3476169 + 0.3162897d*E for this W UMa variable. It is classified as a contact variable with a mean V magnitude of 11.77 and amplitude of V ~ 0.4. Twenty-four times of minimum light are found in the literature along with 3 visual timings. From our present observations, which include four primary eclipses and three secondary eclipses. From these we determined a linear and a quadratic ephemeris, JD Hel MinI = 2459027.65873 ± 0.00080d + 0.31629036 ± 0.00000072×E (1) JD Hel MinI = 2459027.66132 ± 0.00054d + 0.31629221 ± 0.00000017×E+ 0.000000000121 ± 0.000000000011×E2 (2) Thus, from our 16-year period study, the period is found to be increasing. This could be due to mass transfer making the mass ratio decrease (q = M2/M1, all pairs of values should be corrected with a Phase Shift of 0.5). A Wilson-Devinney analyses reveal that the system is an W-type (less massive component is the hottest) W UMa binary with a fairly extreme mass ratio, q = 0.2426 ± 0.0003, 1/q = M1/M2 = 4.1). Its Roche Lobe fill-out is ~23%. One hot spot was needed in the solution. The temperature difference of the components is only ~263 K, with the more massive component as the slightly cooler one. The inclination is high, 87.0 ± 0.2 resulting in a time of constant light in the primary eclipse. The eclipse duration is some 34 minutes. More information is given in this preliminary report.