Journal
PHYSICAL REVIEW C
Volume 102, Issue 4, Pages -Publisher
AMER PHYSICAL SOC
DOI: 10.1103/PhysRevC.102.045808
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Funding
- US National Science Foundation [PHY-1565546]
- US Department of Energy (Office of Science) [DE-SC0014530, DE-NA0002923, DE-SC001920]
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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.
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