  We use a Bayesian inference analysis to explore the sensitivity of Taylor
expansion parameters of the nuclear equation of state (EOS) to the neutron star
dimensionless tidal deformability ($\Lambda$) on 1 to 2 solar masses neutron
stars. A global power law dependence between tidal deformability and
compactness parameter (M/R) is verified over this mass region. To avoid
superfluous correlations between the expansion parameters, we use a
correlation-free EOS model based on a recently published meta-modeling
approach. We find that assumptions in the prior distribution strongly influence
the constraints on $\Lambda$. The $\Lambda$ constraints obtained from the
neutron star merger event GW170817 prefer low values of $L_\text{sym}$ and
$K_\text{sym}$, for a canonical neutron star with 1.4 solar mass. For neutron
star with mass $<1.6$ solar mass, $L_\text{sym}$ and $K_\text{sym}$ are highly
correlated with the tidal deformability. For more massive neutron stars, the
tidal deformability is more strongly correlated with higher order Taylor
expansion parameters.
