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Atmospheric modeling is used to build synthetic spectral energy distributions(SEDs) for the individual components of the speckle interferometric binarysystem HD375. These synthetic SEDs are combined together for the entire systemand compared with its observational SED in an iterated procedure to achieve thebest fit. Kurucz blanketed models with the measurements of magnitudedifferences were used to build these SED's. The input physical elements forbuilding these best fitted synthetic SEDs represent adequately enough theelements of the system. These elements are: $T_{\rm eff}^{a} =6100\pm50$\,K,$T_{\rm eff}^{b} =5940\pm50$\,K, log $g_{a}=4.01\pm0.10$, log$g_{b}=3.98\pm0.10$, $R_a=1.93\pm0.20 R_\odot$, $R_b=1.83\pm0.20 R_\odot$$M_{v}^{\rm a}=3.26\pm0.40$, $M_{v}^{\rm b}=3.51\pm0.50$, $L_a= 4.63\pm0.80L_\odot$ and $ L_b= 3.74\pm0.70 L_\odot$ depending on new estimated parallax$\pi=12.02 \pm 0.60$ mas. A modified orbit of the system is built and comparedwith earlier orbits and the masses of the two components are calculated as $M_a=1.35M_{\odot}$ and $M_b=1.25M_{\odot}$. Depending on the estimated physicaland geometrical elements of the system, which are assured by syntheticphotometry, we suggest that the two components are evolved subgiant (F8.5 IV &G0 IV) stars with age of 3.5 Gy formed by fragmentation.

The visually close binary system HD375; Is it a sub-giant binary?