Are all Equations of State in Neutron Stars born alike?

We have recently provided the generic band of equations of state for matter at attainable densities in zero- and finite-temperature neutron stars restricted only by hadronic physics and fundamental principles, which are crucial for testing General Relativity and theories beyond it. We also characterize any first-order phase transitions therein by the specific latent heat, which we have systematically explored with these EoS for different interpolations. In addition, we used these GR-independent equations of state to constrain the quadratic Palatini gravity f(R). In this work, we incorporate an EoS based on no potential, rather directly from nucleon scattering data [1] for pure neutron matter (PNM) at zero temperature and very low densities by interpolation up to known higher-density physics, applying causality, monotonicity and thermal consistency, in two steps. We use a first interpolation between the uncertainty band obtained for PNM and the saturation density, constrained by nuclear experiments. Then, we use a second interpolation between this band and the high-density perturbative QCD regime and so we cover number densities in the range 10−8 ≤ 𝑛 ≤ 7 fm−3.