ABSTRACT A major source of uncertainty in modelling the strangeness-rich interiors of neutron stars arises from the poorly constrained two-body and three-body interactions among hyperons and nucleons. We perform a comprehensive Bayesian analysis of the and N interaction parameters within the Skyrme Hartree–Fock framework, constrained by both hypernuclei experimental data and astrophysical observations. Our results show that the parameter space of the interaction is tightly constrained by combining nuclear and astrophysical data, while the parameters of the N three-body interaction remain sensitive to astrophysical inputs alone. Specifically, the local, momentum-independent two-body interaction parameter ₀ is tightly constrained and predominantly attractive, while the momentum-dependent parameters ₁ and ₂ contribute repulsive effects at high densities. A key role is played by the potential depth in pure matter, which effectively constrains the two-body interaction and governs the balance between attraction at low densities and repulsion at high densities. The repulsive components of interactions then decrease hyperon fractions and reconcile hyperon-rich equations of state with the observed 2\, M neutron stars, increasing the maximum mass by up to 22 percent. The inclusion of N three-body forces further stiffens the equation of state, raising the maximum mass by up to 0. 1\, M. Our study represents a promising step towards a complete, experimentally grounded description of dense matter across a wide range of densities and strangeness compositions.
Sun et al. (Fri,) studied this question.