Fig. 8: Comparison to nuclear-matter models.
From: Strongly interacting matter exhibits deconfined behavior in massive neutron stars
a The physical quantities displayed in Figs. 1, 2, but this time including as the thin lines all purely hadronic (T = 0, β-equilibrium) models available on the CompOSE database90. The coloring of the individual EoSs corresponds to the relative likelihoods of the models in comparison with the most likely EoS from the GP ensemble. This likelihood depends only on the astrophysical and high-density pQCD inputs. The pQCD constraint is imposed at the TOV points where these curves end, and is implemented by testing whether these points can be connected to the pQCD limit at 40ns in a causal and thermodynamically consistent fashion. The solid red vertical lines here represent the ranges displayed in Table 1, and the dark and light red regions in the background correspond to our \({c}_{s,4}^{2}\) interpolation results. b The normalized pressure of Fig. 4, but including now also the purely hadronic (T = 0, β-equilibrium) model EoSs displayed in panel a. The curves are again set to end at the respective TOV points.
