We present a comprehensive set of physical and geometrical parameters for each of the components of the close visual binary system HIP 11253 (HD 14874). We present an analysis for the binary and multiple stellar systems with the aim to obtain a match between the overall observational spectral energy distribution of the system and the spectral synthesis created from model atmospheres using Al-Wardat's method for analyzing binary and multiple stellar systems. The epoch positions are used to determine the orbital parameters and the total mass. The parameters of both components are derived as: \(T^{\rm a}_{\rm eff}=6025, T_{\rm eff}^{\rm b}=4710,\) logga = 4.55, loggb = 4.60, Ra = 1.125 R⊙, Rb = 0.88 R⊙, La = 1.849 L⊙, Lb = 0.342 L⊙. Our analysis shows that the spectral types of the components are F9 and K3. By combining the orbital solution with the parallax measurements of Gaia DR2 and EDR3, we estimate the individual masses using the H-R diagram as Ma = 1.09 M⊙ and Mb = 0.59 M⊙ for using Gaia DR2 parallax and Ma = 1.10 M⊙ and Mb = 0.61 M⊙ for using Gaia EDR3 parallax. Finally, the location of both system's components on the stellar evolutionary tracks is presented.