The composition and properties of infinite nuclear matter under extreme conditions of temperature and pressure remain incompletely understood. In this work, we constrain the equation of state (EoS) of nuclear matter—constructed within the framework of the relativistic mean field (RMF) model—by combining results from chiral effective field theory and multimessenger observations of neutron stars. Using the saturation properties of nuclear matter, we generate a wide ensemble of EoS, which are subsequently constrained within a Bayesian framework. The resulting posterior distributions provide tight bounds on both the saturation parameters and the coupling constants of the RMF model. The radius of a $1.4M_{\odot }$ neutron star is tightly constrained to ${12.471}_{-0.394}^{+0.427}\mathrm{km}$, while the maximum mass reaches ${2.156}_{-0.120}^{+0.175}{M}_{\odot }$. Furthermore, our analysis reveals that the $\omega –\rho$ coupling, which governs the density dependence of the symmetry energy, becomes increasingly significant under successive astrophysical constraints. Finally, the predicted ${\mathrm{r}}_{\mathrm{skin}}$ of ${}^{48}\mathrm{Ca}$ agrees well with the CREX measurement, whereas that of ${}^{208}\mathrm{Pb}$ remains in tension with PREX-II. In contrast to earlier studies, we do not observe a clear correlation between the ${\mathrm{r}}_{\mathrm{skin}}$ of ${}^{208}\mathrm{Pb}$ and the symmetry energy slope parameter $L$.

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• Gravitational waves
• Neutron skin thickness
• Nuclear matter in neutron stars