TL;DR
This paper explores holographic models for dense QCD matter, suggesting that the deconfinement transition influences neutron star maximum mass and proposing a unified strong coupling framework for nuclear and quark matter phases.
Contribution
It introduces a model that unifies nuclear and quark matter phases at strong coupling, providing insights into neutron star structure and phase transitions.
Findings
Deconfinement phase transition impacts neutron star maximum mass
Nuclear matter is stiff, likely excluding quark cores in neutron stars
Caution advised when simulating neutron star mergers with beyond-ideal fluid corrections
Abstract
The holographic models for dense QCD matter work surprisingly well. A general implication seems that the deconfinement phase transition dictates the maximum mass of neutron stars. The nuclear matter phase turns out to be rather stiff which, if continuously merged with nuclear matter models based on effective field theories, leads to the conclusion that neutron stars do not have quark matter cores in the light of all current astrophysical data. We comment that as the perturbative QCD results are in stark contrast with strong coupling results, any future simulations of neutron star mergers incorporating corrections beyond ideal fluid should proceed cautiously. For this purpose, we provide a model which treats nuclear and quark matter phases in a unified framework at strong coupling.
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