This study outlines a detailed investigation using CCD UBV and Gaia DR3 data sets of the two open clusters Ruprecht 1 (Rup-1) and Ruprecht 171 (Rup-171). Fundamental astrophysical parameters such as color excesses, photometric metallicities, ages, and isochrone distances were based on UBV-data analyses, whereas membership probability calculations, structural and astrophysical parameters, as well as the kinematic analyses were based on Gaia DR3-data. We identified 74 and 596 stars as the most probable cluster members with membership probabilities over 50% for Rup-1 and Rup-171, respectively. The color excesses E(B-V) were obtained as 0.166+/-0.022 and 0.301+/-0.027mag for Rup-1 and Rup-171, respectively. Photometric metallicity analyses were performed by considering F-G type main-sequence member stars and found to be [Fe/H]=-0.09+/-0.16 and [Fe/H]=-0.20+/-0.20dex for Rup-1 and Rup-171, respectively. Ages and distances were based on both UBV and Gaia-data analyses; according to isochrone-fitting these values were estimated to be t=580+/-60Myr, d=1469+/-57pc for Rup-1 and t=2700+/-200Myr, d=1509+/-69pc for Rup-171. The present-day mass function slope of Rup-1 was estimated as 1.26+/-0.32 and Rup-171 as 1.53+/-1.49. Galactic orbit integration analyses showed that both of the clusters might be formed outside the solar circle.