  The impacts of various symmetry energy parameters on the properties of
neutron stars (NSs) have been recently investigated, and the outcomes are at
variance, as summarized in Table III of Phys. Rev. D 106, 063005 (2022). We
have systematically analyzed the correlations of slope and curvature parameters
of symmetry energy at the saturation density ($\rho_0=0.16 \text{fm}^{-3}$)
with the tidal deformability and stellar radius of non-spinning neutron stars
in the mass range of $1.2 - 1.6 M_\odot$ using a large set of minimally
constrained equations of state (EoSs). The EoSs at low densities correspond to
the nucleonic matter and are constrained by empirical ranges of a few low-order
nuclear matter parameters from the finite nuclei data and the pure neutron
matter EoS from chiral effective field theory. The EoSs at high densities
($\rho > 1.5 - 2\rho_0$) are obtained by a parametric form for the speed of
sound that satisfies the causality condition. Several factors affecting the
correlations between the NS properties and the individual symmetry energy
parameters usually encountered in the literature are considered. These
correlations are quite sensitive to the choice of the distributions of symmetry
energy parameters and their interdependence. But, variations of NS properties
with the pressure of $\beta -$ equilibrated matter at twice the saturation
density remain quite robust which maybe due to the fact that the pressure
depends on the combination of multiple nuclear matter parameters that describe
the symmetric nuclear matter as well as the density dependence of the symmetry
energy. Our results are practically insensitive to the behavior of EoS at high
densities.
