  The data release DR2 of Gaia mission was of great help in precise
determination of fundamental parameters of Close Visual Binary and Multiple
Systems (CVBMSs), especially masses of their components, which are crucial
parameters in understating formation and and evolution of stars and galaxies.
This article presents the complete set of fundamental parameters of two nearby
(CVBSs), these are HIP 19206 and HIP 84425. We used a combination of two
methods; the first one is Tokovinin's dynamical method to solve the orbit of
the system and to estimate orbital elements and the dynamical mass sum, and the
second one is Al-Wardat's method for analyzing CVBMSs to estimate the physical
parameters of the individual components. The latest method employs grids of
Kurucz line-blanketed plane parallel model atmospheres to build synthetic
Spectral Energy Distributions (SED) of the individual components. Trigonometric
parallax measurements given by Gaia DR2 and Hipparcos catalogues are used to
analyse the two systems. The difference in these measurements yielded slight
discrepancies in the fundamental parameters of the individual components
especially masses. So, a new dynamical parallax is suggested in this work based
on the most convenient mass sum as given by each of the two methods. The new
dynamical parallax for the system Hip 19205 as $22.97\pm 0.95$ mas coincides
well with the trigonometric one given recently (in December 2020) by Gaia DR3
as $22.3689\pm 0.4056$ mas.
  The positions of the components of the two systems on the evolutionary tracks
and isochrones are plotted, which suggest that all components are solar-type
main sequence stars. Their most probable formation and evolution scenarios are
also discussed.
