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Constraining neutron star matter with QCD
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Constraining neutron star matter with QCD
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In recent years, there have been several successful attempts to constrain the equation of state of neutron star matter using input from low-energy nuclear physics and observational data. We demonstrate that significant further restrictions can be placed by additionally requiring the pressure to approach that of deconfined quark matter at high densities. Remarkably, the new constraints turn out to be highly insensitive to the amount --- or even presence --- of quark matter inside the stars.
Forward citations
Cited by 8 Pith papers
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Strongly Interacting Dark Matter admixed Neutron Stars
Strongly interacting dark matter described by a first-principles G2 gauge-theory equation of state can be mixed into neutron stars while remaining compatible with current observational constraints.
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Modified-excluded-volume EOS with continuous van der Waals phase transition yields CCSN explosions and a several-millisecond neutrino burst, while the same EOS under Gibbs construction fails to explode.
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Requiring causal stable thermodynamically consistent extensions of neutron-star EOS models to perturbative QCD constrains high-density behavior and disfavors purely nucleonic descriptions for all stable stars.
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One-loop HDL thermodynamics of a strongly magnetized isospin asymmetric cold quark matter
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Quark and hybrid stars with renormalization group improvement of NNLO perturbative QCD
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A textbook-style review of the neutron-star equation of state covering the models, experimental and observational constraints, and open questions, with no new result claimed or derived.
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