## Abstract

We delineate the properties of QCD matter at baryon density n_{B}=1−10n_{0} (n_{0}: 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 n_{B}≲2n_{0} purely nuclear matter; at n_{B}≳5n_{0} percolated quark matter; and at 2n_{0}≲n_{B}≲5n_{0} 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 n_{B}=1−10n_{0} remain non-perturbative even after quark matter formation.

Original language | English |
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Pages (from-to) | 821-825 |

Number of pages | 5 |

Journal | Nuclear Physics A |

Volume | 956 |

DOIs | |

Publication status | Published - 2016 Dec 1 |

## Keywords

- Neutron stars
- QCD equations of state