Astronomical and terrestrial studies on the equation of state of dense matter

Quantitatively determining the equation of state (EOS) of dense matter remains a forefront challenge at the intersection of nuclear physics and astrophysics. To overcome limitations in both theory and experiment, the present study utilizes nucleon interaction information extracted from terrestrial nuclear experiments, in combination with nuclear many-body theory and non-equilibrium transport models, and incorporates high-precision astrophysical observations of neutron stars to constrain the fundamental properties of dense nuclear matter in their cores. Specifically, we perform a self-consistent joint analysis that integrates collective flow and pion production data from heavy-ion collisions with neutron star observables, including mass, radius, and tidal deformability. Using Bayesian inference with multi-dimensional datasets, we obtain updated constraints on key EOS parameters at nuclear saturation density (with 1σ credible intervals): the incompressibility K_0 = 250.56^+16.51-18.79 rm MeV, nucleon effective mass ratio m^*/m = 0.6^+0.01-0.01 symmetry energy S_0 = 28.46^+4.36-2.24 rm MeV, and symmetry energy slope L_0 = 64.59^+13.25-9.38 rm MeV. In addition, this study identifies the observables most sensitive to these parameters, providing valuable guidance and theoretical support for future efforts to jointly constrain the EOS through high-precision nuclear experiments and astrophysical observations.