Impact of the neutron-star deformability on equation of state parameters

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$_{\mathrm{sym}}$ and K$_{\mathrm{sym}}$, for a canonical neutron star with 1.4 solar mass. For neutron star with mass \textless 1.6 solar mass, L$_{\mathrm{sym}}$ and K$_{\mathrm{sym}}$ 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.