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Atmospheric modelling of the components of the visually close binary systemsHip70973 and Hip72479 was used to estimate the individual physical parametersof their components. The model atmospheres were constructed using a grid ofKurucz solar metalicity blanketed models, and used to compute a syntheticspectral energy distribution for each component separately, and hence for thecombined system. The total observational spectral energy distributions of thesystems were used as a reference for the comparison with the synthetic ones. Weused the feedback modified parameters and iteration method to get the best fitbetween synthetic and observational spectral energy distributions. The physicalparameters of the components of the system Hip70973 were derived as: Ta eff =5700{\pm}75 K, Tb eff = 5400{\pm}75 K, log ga = 4.50{\pm}0.05, log gb =4.50{\pm}0.05, Ra = 0.98{\pm}0.07R{\odot}, Rb = 0.89{\pm}0.07R{\odot}, and pi =26.25 {\pm} 1.95 mas, with G4 & G9 spectral types. And those of the systemHip72479 as: Ta eff = 5400 {\pm} 50 K, Tb eff = 5180 {\pm} 50 K, log ga = 4.50{\pm} 0.05, log gb = 4.60 {\pm} 0.05, Ra = 0.89 {\pm} 0.07R{\odot}, Rb = 0.80{\pm} 0.07R{\odot}, and pi = 23.59 {\pm} 1.00 mas with G9 & K1 spectral types.

Physical Parameters of the Visually Close Binary Systems Hip70973 and Hip72479