  The nuclear symmetry energy plays important role on the structure of finite
nuclei as well as on the bulk properties of neutron stars. However, its values
at high densities are completely uncertain and the corresponding experimental
data have a large error. One possibility to determine or at least estimate the
values at high densities is with the help of neutron star observations.
Recently, observations of gravitational waves from merging processes of binary
neutron star systems provide useful information on both their radius and tidal
deformability, quantities directly related to the symmetry energy. In this
work, an attempt is made in this direction, namely to see how recent
observations can help to constrain the structure of finite nuclei. In
particular, in the present study we parameterize the equation of state which
describes the asymmetric and symmetric nuclear mater with the help of the
parameter $\eta=(K_0 L^2)^{1/3}$, where $K_0$ is the incompressibility and $L$
the slope parameter. The parameter $\eta$ is a regulator of the stiffness of
the equation of state. We expect that the values of $\eta$ affect both the
properties of finite nuclei as well as of the neutron star properties (where
the role of the isovector interaction plays important role). It is natural to
expect that constraints, via the parameter $\eta$ on finite nuclei will imply
constraints on the neutron star properties and vice versa. In view of the above
statements we propose a simple but self-consistent method to examine
simultaneously the effects of the parameter $\eta$ on the properties of finite
nuclei and neutron stars. We found constraints on the latter systems via
combination by the recent experiments (PREX-2) and observational data found by
the detectors Ligo and Virgo.
