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 (A) on 1- to 2-solar-mass neutron stars. A global power law dependence between tidal deformability and the 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 metamodeling approach. We find that assumptions in the prior distribution strongly influence the constraints on A. The A constraints obtained from the neutron star merger event GW170817 prefer low values of L-sym and K-sym, for a canonical neutron star with 1.4 solar masses. For a neutron star with mass <1.6 solar masses, L-sym and K-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.