  The visually close binary system HD25811 is analyzed to estimate its physical
and geometrical parameters in addition to its spectral type and luminosity
class. The method depends on obtaining the best fit between the entire
observational spectral energy distribution (SED) of the system and synthetic
SEDs created by atmospheric modeling of the individual components, consistent
with the system's modified orbital elements. The parameters of the individual
components of the system are derived as: $T_{\rm eff}^{\rm a} =6850\pm50$\,K,
$T_{\rm eff}^{\rm b} =7000\pm50$\,K, log $g_{\rm a}=4.04\pm0.10$, log $g_{\rm
b}=4.15\pm0.10$, $R_{\rm a}=1.96\pm0.20$\,R$_{\odot}$, $R_{\rm
b}=1.69\pm0.20$\,R$_{\odot}$, $M_{va}=1.97\pm0.20$, $M_{vb}=2.19\pm0.20$, $L_a=
7.59\pm0.70 L_\odot, L_b= 6.16\pm0.70 L_\odot$ with dynamical parallax
$\pi(\textrm{mas})=5.095\pm 0.095$. The analysis shows that the system consists
of a $1.55M_{\odot}$ F2 primary star and a less evolved $1.50M_{\odot}$ F1
secondary subgiant star with ages around 2 Gy formed by fragmentation.
Synthetic magnitudes of both components were calculated under Johnson-Cousins,
Str\"{o}mgren, and Tycho photometrical systems.
