Abstract
We delineate the properties of QCD matter at baryon density nB=1−10n0 (n0: nuclear saturation density), through the construction of neutron star equations of state that satisfy the neutron star mass-radius constraints as well as physical conditions on the speed of sound. The QCD matter is described in the 3-window modeling: at nB≲2n0 purely nuclear matter; at nB≳5n0 percolated quark matter; and at 2n0≲nB≲5n0 matter intermediate between these two which are constructed by interpolation. Using a schematic quark model with effective interactions inspired from hadron and nuclear physics, we analyze the strength of interactions necessary to describe observed neutron star properties. Our finding is that the interactions should remain as strong as in the QCD vacuum, indicating that gluons at nB=1−10n0 remain non-perturbative even after quark matter formation.
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