  We present the stellar parameters of the individual components of the two old
close binary systems HIP\,14075 and HIP\,14230 using synthetic photometric
analysis. These parameters are accurately calculated based on the best match
between the synthetic photometric results within three different photometric
systems with the observed photometry of the entire system. From the synthetic
photometry, we derive the masses and radii of HIP\,14075 as:
$\mathcal{M}^A=0.99\pm0.19\, \mathcal{M_\odot}$, $R_{A}=0.877\pm0.08\, R_\odot$
for the primary and $\mathcal{M}^B=0.96\pm0.15\, \mathcal{M_\odot}$,
$R_{B}=0.821\pm0.07\, R_\odot$ for the secondary, and of HIP\,14230 as:
$\mathcal{M}^A=1.18\pm0.22\, \mathcal{M_\odot}$, $R_{A}=1.234\pm0.05\, R_\odot$
for the primary and $\mathcal{M}^B=0.84\pm0.12\, \mathcal{M_\odot}$,
$R_{B}=0.820\pm0.05\, R_\odot$ for the secondary, both systems depend on Gaia
parallaxes. Based on the positions of the components of the two systems on a
theoretical Hertzsprung- Russell diagram, we find that the age of HIP 14075 is
$11.5\pm2.0$\,Gyr and of HIP 14230 is $3.5\pm1.5$\,Gyr. Our analysis reveals
that both systems are old close binary systems ($\approx >$ 4 Gyr). Finally,
the positions of the components of both systems on the stellar evolutionary
tracks and isochrones are discussed.
