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We use a Bayesian inference analysis to explore the sensitivity of Taylorexpansion parameters of the nuclear equation of state (EOS) to the neutron stardimensionless tidal deformability ($\Lambda$) on 1 to 2 solar masses neutronstars. A global power law dependence between tidal deformability andcompactness parameter (M/R) is verified over this mass region. To avoidsuperfluous correlations between the expansion parameters, we use acorrelation-free EOS model based on a recently published meta-modelingapproach. We find that assumptions in the prior distribution strongly influencethe constraints on $\Lambda$. The $\Lambda$ constraints obtained from theneutron 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 neutronstar with mass $<1.6$ solar mass, $L_\text{sym}$ and $K_\text{sym}$ are highlycorrelated with the tidal deformability. For more massive neutron stars, thetidal deformability is more strongly correlated with higher order Taylorexpansion parameters.

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