  Atmospheric modelling of the components of the visually close binary systems
Hip70973 and Hip72479 was used to estimate the individual physical parameters
of their components. The model atmospheres were constructed using a grid of
Kurucz solar metalicity blanketed models, and used to compute a synthetic
spectral energy distribution for each component separately, and hence for the
combined system. The total observational spectral energy distributions of the
systems were used as a reference for the comparison with the synthetic ones. We
used the feedback modified parameters and iteration method to get the best fit
between synthetic and observational spectral energy distributions. The physical
parameters 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 system
Hip72479 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.
