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.
Cold Quark Matter
9 Pith papers cite this work. Polarity classification is still indexing.
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Pith papers citing it
abstract
We perform an O(alpha_s^2) perturbative calculation of the equation of state of cold but dense QCD matter with two massless and one massive quark flavor, finding that perturbation theory converges reasonably well for quark chemical potentials above 1 GeV. Using a running coupling constant and strange quark mass, and allowing for further non-perturbative effects, our results point to a narrow range where absolutely stable strange quark matter may exist. Absent stable strange quark matter, our findings suggest that quark matter in compact star cores becomes confined to hadrons only slightly above the density of atomic nuclei. Finally, we show that equations of state including quark matter lead to hybrid star masses up to M~2M_solar, in agreement with current observations. For strange stars, we find maximal masses of M~2.75M_solar and conclude that confirmed observations of compact stars with M>2M_solar would strongly favor the existence of stable strange quark matter.
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Non-parametric EOS construction from crust to pQCD forces a sound-speed peak and softening that realizes a generalized quark-hadron crossover in massive neutron stars.
Amortized neural posterior estimation reproduces nested sampling constraints on RMF couplings for neutron-star EOS with no bias and generates 30,000 samples in 2.5 seconds.
With current multi-messenger EOS constraints, the post-merger peak frequency f2,mean is determined to ~100 Hz at fixed mass and tidal deformability/radius, tight enough to expose thermal or phase-transition physics.
RGOPT-resummed NNLO pQCD EoS for massive quarks in beta equilibrium is fitted and applied to construct pure quark stars (X=3.08-3.58) and hybrid stars (X~2-2.98) compatible with PSR J0740+6620 and GW190814.
Hybrid neutron-star equations of state remain sensitive to the low-density nucleonic model at transition densities around 2ρ₀, with model spread in radius and tidal deformability exceeding observational uncertainty by factors of ~1.8 and ~1.4.
In a constructed QCD equation of state incorporating surface energy, critical exponents require temperature within 1% of the critical value, casting doubt on their measurability in heavy ion experiments.
The IdylliQ model uses quark saturation to generate stiff equations of state and effective baryon repulsions that mitigate hyperon softening in neutron star matter.
A mass-dependent renormalization scheme from dimensional regularization yields smooth threshold transitions in QCD and implements the Appelquist-Carazzone theorem by reducing to minimal subtraction at high energies.
citing papers explorer
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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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The Non-parametric Equation of State Realizes a Generalized Quark-Hadron Crossover
Non-parametric EOS construction from crust to pQCD forces a sound-speed peak and softening that realizes a generalized quark-hadron crossover in massive neutron stars.
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Amortized Simulation-Based Inference of Relativistic Mean-Field Couplings for Neutron-Star Equations of State
Amortized neural posterior estimation reproduces nested sampling constraints on RMF couplings for neutron-star EOS with no bias and generates 30,000 samples in 2.5 seconds.
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Post-Merger Gravitational-Wave Uncertainties of Binary Neutron Stars under Multi-Messenger EOS Constraints
With current multi-messenger EOS constraints, the post-merger peak frequency f2,mean is determined to ~100 Hz at fixed mass and tidal deformability/radius, tight enough to expose thermal or phase-transition physics.
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Quark and hybrid stars with renormalization group improvement of NNLO perturbative QCD
RGOPT-resummed NNLO pQCD EoS for massive quarks in beta equilibrium is fitted and applied to construct pure quark stars (X=3.08-3.58) and hybrid stars (X~2-2.98) compatible with PSR J0740+6620 and GW190814.
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Sensitivity of Neutron Star Observables to Transition Density in Hybrid Equation-of-State Models
Hybrid neutron-star equations of state remain sensitive to the low-density nucleonic model at transition densities around 2ρ₀, with model spread in radius and tidal deformability exceeding observational uncertainty by factors of ~1.8 and ~1.4.
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Scaling of the Surface Free Energy as a Probe of the QCD Critical Region
In a constructed QCD equation of state incorporating surface energy, critical exponents require temperature within 1% of the critical value, casting doubt on their measurability in heavy ion experiments.
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A quarkyonic matter model
The IdylliQ model uses quark saturation to generate stiff equations of state and effective baryon repulsions that mitigate hyperon softening in neutron star matter.
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Smooth Threshold Effects from Dimensional Regularization
A mass-dependent renormalization scheme from dimensional regularization yields smooth threshold transitions in QCD and implements the Appelquist-Carazzone theorem by reducing to minimal subtraction at high energies.