Ab-initio QCD calculations impact the inference of the neutron-star-matter equation of state

Gorda, Tyler; Komoltsev, Oleg; Kurkela, Aleksi

doi:10.48550/arxiv.2204.11877

Cited by 21 publications

(68 citation statements)

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“…We would remind that the ab initio constraints have not been properly taken into account for any gravitational wave simulations (see Ref. [44] for the latest analysis of the ab initio constraints). Because QCD is the most fundamental theory, if the density is high enough to justify the perturbative expansion, the genuine EOS must eventually meet the quark branch from pQCD.…”

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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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“…Still, on a qualitative level, the density dependence of the speed of sound in neutron-star matter may also be constrained by mechanisms which are similar to the ones discussed in the present work. Indeed, with respect to the maximum in the speed of sound, constraints from neutron-star masses also strongly support the existence of a maximum in the speed of sound in neutron-rich matter [13][14][15][16][17][18][19]. In particular, the existence of a maximum in the speed of sound and a local minimum in the speed of sound at high densities has already been discussed in an analysis of constraints from astrophysical observations in Ref.…”

Section: Discussionmentioning

confidence: 80%

“…In recent studies based on the functional renormalization group (fRG) approach, it has then been found that the presence of a color-superconducting gap in the excitation spectrum of the quarks gives rise to a maximum in the speed of sound [23,47,48]. Notably, in accordance with constraints from nuclear physics and observations [13][14][15][16][17][18][19], this maximum exceeds the asymptotic value associated with the non-interacting quark gas, for both isospin-symmetric matter and neutron-star matter.…”

Section: Introductionmentioning

confidence: 80%

“…The impressive progress made in the observation of neutron-star mergers via gravitational-wave signals [1,2] together with the advances made in direct measurements of the radius and the mass of heavy neutron stars [3][4][5][6][7][8][9][10][11][12] challenges our understanding of the properties of dense strong-interaction matter. For example, constraints from neutron-star masses suggest the existence of a maximum in the speed of sound in dense matter which exceeds the asymptotic value of a non-interacting quarks gas [13][14][15][16][17][18][19], preferably at densities n/n 0 10 (where n 0 is the nuclear saturation density).…”

Section: Introductionmentioning

confidence: 99%

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Speed of sound in dense strong-interaction matter

Braun¹,

Geißel²,

Schallmo³

2022

Preprint

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“…Author comments: While finishing this study, a new paper appeared studying the impact of pQCD calculations on the inference of the NS EoS [55], but indicating a larger impact of pQCD as compared to our results. Since we found that pQCD is on the brink of being constraining, it is not surprising that small differences in the treatment lead to larger differences in the conclusions.…”

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confidence: 67%

Perturbative QCD and the Neutron Star Equation of State

Somasundaram¹,

Tews²,

Margueron³

2022

Preprint

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We construct a physics-agnostic approach based on the sound speed model, which connects both low-density information from nuclear theory and high-density constraints from perturbative QCD (pQCD). Using this approach, we study the impact of pQCD constraints on neutron star (NS) equations of state (EoS) that have been constrained by astrophysical observations. We find that the pQCD constraints affect the EoS mainly beyond the densities realized in NS. Furthermore, we observe an interesting interplay between pQCD and astrophysical constraints, with pQCD preferring softer EoS for the heaviest NS while recent NICER observations suggest the EoS to be stiffer. We explore the sensitivity of our findings to pQCD uncertainties and we study the constraining power of pQCD if future observations of heavy NS were to suggest radii larger than 13 km for heavy stars.

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Ab-initio QCD calculations impact the inference of the neutron-star-matter equation of state

Cited by 21 publications

References 0 publications

Gravitational Wave Signal for Quark Matter with Realistic Phase Transition

Gravitational Wave Signal for Quark Matter with Realistic Phase Transition

Speed of sound in dense strong-interaction matter

Perturbative QCD and the Neutron Star Equation of State

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