How Perturbative QCD Constrains the Equation of State at Neutron-Star Densities

Komoltsev, Oleg; Kurkela, Aleksi

doi:10.1103/physrevlett.128.202701

Cited by 73 publications

(71 citation statements)

References 68 publications

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“…All technical details as well as analytical formulas are presented in [13]. In this section I describe the conditions I use, in particular stability, consistency and causality, and the resulting propagation of the pQCD input down to lower densities.…”

Section: Setupmentioning

confidence: 99%

“…In this work I answer why and how pQCD input offers significant information about the EOS at NS densities. I find that pQCD input propagates non-trivial constraints all the way down to 2.2n s just by using solely thermodynamic stability, consistency and causality [13]. In addition the complementariness of the pQCD input to the astrophysical observations was studied in [14].…”

Section: Introductionmentioning

confidence: 99%

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QCD in the cores of neutron stars

Komoltsev¹

2022

Preprint

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I discuss why state-of-the art perturbative QCD calculations of the equation of state at large chemical potential that are reliable at asymptotically high densities constrain the same equation of state at neutron-star densities. I describe how these theoretical calculations affect the EOS at lower density. I argue that the ab-initio calculations in QCD offer significant information about the equation of state of the neutron-star matter, which is complementary to the current astrophysical observations.

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Section: Setupmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

QCD in the cores of neutron stars

Komoltsev¹

2022

Preprint

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“…It was shown that imposing complementary limiting constraints at high densities from pQCD in addition to low-density nuclear matter from CEFT reduces the uncertainty of NS matter significantly (Kurkela et al 2014;Komoltsev & Kurkela 2022). The highest observed NS mass ∼ 2 M (Demorest et al 2010;Antoniadis et al 2013;Cromartie et al 2020;) further imposes important consequences on the speed of sound for a given EoS.…”

Section: Introductionmentioning

confidence: 99%

Constraining the equation of state of hybrid stars using recent information from multidisciplinary physics

Shirke¹,

Ghosh²,

Chatterjee³

2022

Preprint

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At the ultra-high densities existing in the core of neutron stars, it is expected that a phase transition from baryonic to deconfined quark matter may occur. Such a phase transition would affect the underlying equation of state (EoS) as well as the observable astrophysical properties of neutron stars. Comparison of EoS model predictions with astronomical data from multi-messenger signals then provides us an opportunity to probe the behaviour of dense matter. In this work, we restrict the allowed parameter space of EoS models in neutron stars for both nucleonic (relativistic mean field model) and quark matter (bag model) sectors by imposing state-of-the-art constraints from nuclear calculations, multi-messenger astrophysical data and perturbative QCD (pQCD). We systematically investigate the effect of each constraint on the parameter space of uncertainties using a cut-off filter scheme, as well as the correlations among the parameters and with neutron star astrophysical observables. Using the constraints, we obtain limits for maximum NS mass, maximum central density, as well as for NS radii and tidal deformability. Although pQCD constraints are only effective at very high densities, they significantly reduce the parameter space of the quark model. We also conclude that astrophysical data supports high values of the bag parameter B and disfavors the existence of a pure quark matter core in hybrid stars.

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“…Also, newer constraints on the maximum NS mass and a lower limit of the tidal deformability were also inferred [13,14]. Adding the requirement that the equation of state asymptotically approach the regime of perturbative QCD [14][15][16][17][18][19], leads to constraints on the radius of a maximum-mass NS of R max < 13.6 km and Λ 1.4 > 120 [14]. It has also been shown that an EOS with a phase transition can imply 8.53 km < R 1.4 < 13.74 km and Λ 1.4 > 35.5 at the 3 σ level [13].…”

Section: Introductionmentioning

confidence: 99%

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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How Perturbative QCD Constrains the Equation of State at Neutron-Star Densities

Cited by 73 publications

References 68 publications

QCD in the cores of neutron stars

QCD in the cores of neutron stars

Constraining the equation of state of hybrid stars using recent information from multidisciplinary physics

Neutron Star Mergers and the Quark Matter Equation of State

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