This study utilizes “Al-Wardat’s method for analysing binary and multiple stellar systems” to estimate a set of parameters for the binary system Hip70868. The method compares the system’s observational magnitudes, color indices, and spectral energy distribution (SED) and synthetic SEDs generated through atmospheric modeling of each component. Feedback-adjusted parameters and an iterative approach were employed to achieve the best fit between observational (including the latest measurements of Gaia, release DR3) and synthetic spectral energy distributions. The findings were completed using the distance of 71.89 pc given by Hipparcos 2007’s new reduction. The individual components’ parameters for the system were derived afterward. The parameters obtained for the individual components are as follows: Component A has an effective temperature (Teff) of 6072 ± 50 K, a surface gravity (log ga) of 4.50 ± 0.05, and a radius (Ra) of 1.40 ± 0.07 \({\text{R}}_{\odot}\) . Component B has a (Teff) of 5887 ± 50 K, a (log gb) of 4.40 ± 0.05, and a radius (Rb) of 1.326 ± 0.07 \({\text{R}}_{\odot}\) . The spectral types of the components were found to be F9 IV and G1 IV, respectively. The findings from this analysis were utilized to accurately position the two system components on the Hertzsprung-Russell (H-R) diagram and the evolutionary tracks. The analysis shows that the components have transitioned from the main sequence to the sub-giant stage of their evolution.