Binary neutron star mergers as a probe of quark-hadron crossover equations of state

Kedia, Atul; Kim, Hee Il; Suh, In-Saeng; Mathews, Grant J.

doi:10.48550/arxiv.2203.05461

Cited by 3 publications

(17 citation statements)

References 66 publications

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“…From this point of view, the merger simulations with preferable EOS candidates with continuous crossover to QM should be important. Recently, numerical simulations with quark-hadron crossover (QHC) EOSs have been reported [39,40].…”

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confidence: 99%

Gravitational Wave Signal for Quark Matter with Realistic Phase Transition

Fujimoto¹,

Fukui²,

Hotokezaka³

et al. 2022

Preprint

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The cores of neutron stars (NSs) near the maximum mass realize the most highly compressed matter in the universe where quark degrees of freedom may be liberated. Such a state of dense matter is hypothesized as quark matter (QM) and its presence has awaited to be confirmed for decades in nuclear physics. Gravitational waves from binary NS mergers are expected to convey useful information called the equation of state (EOS). However, the signature for QM with realistic EOS is not yet established.Here, we show that the gravitational wave in the post-merger stage can distinguish the theory scenarios with and without a transition to QM. Instead of adopting specific EOSs as studied previously, we compile reliable EOS constraints from the ab initio approaches. We demonstrate that early collapse to a black hole after NS merger signifies softening of the EOS associated with the onset of QM in accord with ab initio constraints. Nature of hadron-quark phase transition can be further constrained by the condition that electromagnetic counterparts need to be energized by the material left outside the remnant black hole.

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confidence: 99%

Gravitational Wave Signal for Quark Matter with Realistic Phase Transition

Fujimoto¹,

Fukui²,

Hotokezaka³

et al. 2022

Preprint

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“…Many models admit to a comparison to versions of the generalized MIT bag model [36] approach and include QCD mean field approximations [37,38] along with computationally intensive numerical lattice approaches that are being improved to accommodate finite-temperature chemical potentials [39]. Refined models include crustal effects [40], deformations [41], layering [42], cooling rates [43], strange quark cores [44], post-merger analysis [45], finite-temperature boson stars [46], kaon condensation [47,48], superconducting color vector potential effects [30,49], phase transitions and different crystalline cores [50][51][52].…”

Section: Introductionmentioning

confidence: 99%

Cold Quark–Gluon Plasma EOS Applied to a Magnetically Deformed Quark Star with an Anomalous Magnetic Moment

Andrew

Steinfelds

Andrew³

2022

Universe

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We consider a QCD cold-plasma-motivated Equation of State (EOS) to examine the impact of an Anomalous Magnetic Moment (AMM) coupling and small shape deformations on the static oblate and prolate core shapes of quark stars. Using the Fogaça QCD-motivated EOS, which shifts from the high-temperature, low-chemical-potential quark–gluon plasma environment to the low-temperature, high-chemical-potential quark stellar core environment, we consider the impact of an AMM coupling with a metric-induced shape deformation parameter in the Tolman–Oppenheimer–Volkov (TOV) equations. The AMM coupling includes a phenomenological scaling that accounts for the weak and strong field characteristics in dense matter. The EOS is developed using a hard gluon and soft gluon decomposition of the gluon field tensor and using a mean-field effective mass for the gluons. The AMM is considered using the Dirac spin tensor coupled to the EM field tensor with quark-flavor-based magnetic moments. The shape parameter is introduced in a metric ansatz that represents oblate and prolate static stellar cores for modified TOV equations. These equations are numerically solved for the final mass and radius states, representing the core collapse of a massive star with a phase transition leading to an unbound quark–gluon plasma. We find that the combined shape parameter and AMM effects can alter the coupled EOS–TOV equations, resulting in an increase in the final mass and a decrease in the final equatorial radius without collapsing the core into a black hole and without violating causality constraints; we find maximum mass values in the range 1.6 Mʘ < M < 2.5 Mʘ. These states are consistent with some astrophysical, high-mass magnetar/pulsar and gravity wave systems and may provide evidence for a core that has undergone a quark–gluon phase transition such as PSR 0943 + 10 and the secondary from the GW 190814 event.

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“…In recent work [1] we have explored the effects of a crossover transition to quark matter on the emergent gravitational waves from binary neutron star mergers. In this paper we summarize that work and other efforts toward unraveling the effects of the formation of quark-matter during neutron-star mergers.…”

Section: Introductionmentioning

confidence: 99%

“…This could extend the postmerger phase. Hence, an observation of a long-duration post-merger GW event, could possibly indicate both the order of the transition and the coupling strength of quark-matter in the crossover regime [1].…”

Section: Introductionmentioning

confidence: 99%

“…In Ref. [1] we examined the crossover to the formation of quark-gluon plasma during the postmerger and demonstrated that the GW signal from the postmerger phase is indeed sensitive to the quark-matter EOS. It was shown that that the properties of quark matter in the non-perturbative crossover regime of QCD increases the pressure of the postmerger remnant.…”

Section: Introductionmentioning

confidence: 99%

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Neutron Star Mergers and the Quark Matter Equation of State

et al. 2022

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As neutron stars merge they can approach very high nuclear density. Here, we summarized recent results for the evolution and gravitational wave emission from binary-neutron star mergers using a a variety of nuclear equations of state with and without a crossover transition to quark matter. We discuss how the late time gravitational wave emission from binary neutron star mergers may possibly reveal the existence of a crossover transition to quark matter.

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Binary neutron star mergers as a probe of quark-hadron crossover equations of state

Cited by 3 publications

References 66 publications

Gravitational Wave Signal for Quark Matter with Realistic Phase Transition

Gravitational Wave Signal for Quark Matter with Realistic Phase Transition

Cold Quark–Gluon Plasma EOS Applied to a Magnetically Deformed Quark Star with an Anomalous Magnetic Moment

Neutron Star Mergers and the Quark Matter Equation of State

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