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Neutron Star vs Quark Star in the Multimessenger Era

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arxiv 2308.16783 v1 pith:PXREODFR submitted 2023-08-31 astro-ph.HE hep-phnucl-exnucl-th

Zheng Cao , Lie-Wen Chen This is my paper · ORCID
classification astro-ph.HEhep-phnucl-exnucl-th
keywords corequarkstarcaseneutronobservedscenariosound
verification ladder T0 review T1 audit T2 compute T3 formal
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abstract

Neutron stars (NSs) which could contain exotic degrees of freedom in the core and the self-bound quark stars (QSs) made purely of absolutely stable deconfined quark matter are still two main candidates for the compact objects observed in pulsars and gravitational wave (GW) events in binary star mergers. We perform a Bayesian model-agnostic inference of the properties of NSs and QSs by combining multi-messenger data of GW170817, GW190425, PSR J0030+0451, PSR J0740+6620, PSR J1614-2230, PSR J0348+0432 as well as ab initio calculations from perturbative quantum chromodynamics and chiral effective field theory. We find the NS scenario is strongly favored against the QS scenario with a Bayes factor of NS over QS $\mathcal{B}^\text{NS}_\text{QS} = 11.5$. In addition, the peak of the squared sound velocity $c_s^2 \sim 0.5c^2$ around $3.5$ times nuclear saturation density $n_0$ observed in the NS case disappears in the QS case which suggests that the $c_s^2$ first increases and then saturates at $c_s^2 \sim 0.5c^2$ above $\sim 4n_0$. The sound velocity and trace anomaly are found to approach the conformal limit in the core of heavy NSs with mass $M \gtrsim 2M_{\odot}$, but not in the core of QSs.

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Cited by 5 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Quarkyonic Stars with Strangeness

    nucl-th 2026-07 conditional novelty 6.0 of 10

    A three-flavor quarkyonic model with octet baryons yields stiffer neutron-star EOS and raises maximum masses, potentially resolving the hyperon puzzle.

  2. High density symmetry energy: A key to the solution of the hyperon puzzle

    nucl-th 2024-11 conditional novelty 6.0 of 10

    A soft-then-stiff symmetry energy delays hyperon appearance and lets hyperon stars reach about 2 solar masses while matching a wide set of astrophysical constraints.

  3. Bayesian constraints on quark stars from multi-messenger observations

    astro-ph.HE 2025-06 conditional novelty 5.0 of 10

    A Bayesian analysis shows quark star models with an interacting MIT bag EOS naturally fit the low-mass object HESS J1731-347, but support for a roughly 2.6 solar mass quark star in GW190814 depends on the chosen priors.

  4. An Effective Upper Bound on the Pressure-to-Energy Density Ratio in Neutron Stars

    nucl-th 2026-01 reject novelty 4.0 of 10

    Using a fitted effective correction in their IPAD-TOV framework, the authors obtain X≲0.385, a looser bound than their earlier 0.374, plus an empirical compactness scaling fit to 284 EOSs.

  5. Novel Scalings of Neutron Star Properties from Analyzing Dimensionless Tolman--Oppenheimer--Volkoff Equations

    astro-ph.HE 2025-01 reject novelty 3.0 of 10

    IPAD-TOV is a perturbative analysis of dimensionless TOV equations yielding claimed EOS-model-independent scalings and a bound X=Pc/εc≤0.374, used to extract central EOS from NS observations.

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