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Observations of neutron stars (NSs) by the LIGO-Virgo and NICERcollaborations have provided reasonably precise measurements of their variousmacroscopic properties. In this paper, we employ a Bayesian framework tocombine them and place improved joint constraints on the properties of NSequation of state (EoS). We use a hybrid EoS formulation that employs aparabolic expansion-based nuclear empirical parameterization around the nuclearsaturation density augmented by a generic 3-segment piecewise polytrope modelat higher densities. Within the $90 \%$ credible level this parameterizationpredicts $R_{1.4} = 12.57_{-0.92}^{+0.73}$ km and $\Lambda_{1.4} =550_{-225}^{+223}$ for the radius and dimensionless tidal deformability,respectively, of a $1.4 M_{\odot}$ NS. Finally, we show how the construction ofthe full NS EoS based solely on the nuclear empirical parameters at saturationdensity leads to certain tension with the astrophysical data, and how thehybrid approach provides a resolution to it.

Towards mitigation of apparent tension between nuclear physics and astrophysical observations by improved modeling of neutron star matter