Constraining quark-hadron interface tension in the multimessenger era

Xia, Caichu; Maruyama, Toshiki; Yasutake, Nobutoshi; Tatsumi, Toshitaka

doi:10.1103/physrevd.99.103017

Cited by 33 publications

(42 citation statements)

References 121 publications

(204 reference statements)

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“…Recent works have placed this surface tension σ HQ > 70 MeV /fm 2 [177,174] which could imply a sharp interface between phases of pure hadronic matter and pure quark matter. In [178] a value σ c = 79.1 MeV/fm 2 has been reported.…”

Section: First Order Phase Transitionmentioning

confidence: 96%

Hadron matter in neutron stars in view of gravitational wave observations

Llanes-Estrada

Lope-Oter

2019

Progress in Particle and Nuclear Physics

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In this review we highlight a few physical properties of neutron stars and their theoretical treatment inasmuch as they can be useful for nuclear and particle physicists concerned with matter at finite density (and newly, temperature). Conversely, we lay out some of the hadron physics necessary to test General Relativity with binary mergers including at least one neutron star, in view of the event GW170817: neutron stars and their mergers reach the highest matter densities known, offering access to the matter side of Einstein's equations. In addition to minimum introductory material for those interested in starting research in the field of neutron stars, we dedicate quite some effort to a discussion of the Equation of State of hadron matter in view of gravitational wave developments; we address phase transitions and how the new data may help; we show why transport is expected to be dominated by turbulence instead of diffusion through most if not all of the star, in view of the transport coefficients that have been calculated from microscopic hadron physics; and we relate many of the interesting physics topics in neutron stars to the radius and tidal deformability.

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Section: First Order Phase Transitionmentioning

confidence: 96%

Hadron matter in neutron stars in view of gravitational wave observations

Llanes-Estrada

Lope-Oter

2019

Progress in Particle and Nuclear Physics

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“…again showing both general and charge neutral expressions. Equations (B5), (B8), and (B11) give the result (29) in the main text.…”

Section: Slabsmentioning

confidence: 99%

“…1 Various levels of approximations have been employed in the literature for mixed phases at the quark-hadron transition. Usually, nuclear and quark matter are treated with two different models [21][22][23][24][25][26][27][28][29][30]. In this approach, the profile of a quark-hadron interface cannot be calculated microscopically since this requires knowledge of an effective potential that connects the two phases.…”

Section: Introductionmentioning

confidence: 99%

Chiral pasta: Mixed phases at the chiral phase transition

Schmitt

2020

Phys. Rev. D

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Interiors of neutron stars are ultradense and may contain a core of deconfined quark matter. Such a core connects to the outer layers smoothly or through a sharp microscopic interface or through an intermediate macroscopic layer of inhomogeneous mixed phases, which is globally neutral but locally contains electrically charged domains. Here I employ a nucleon-meson model under neutron star conditions that shows a first-order chiral phase transition at large densities. In the vicinity of this chiral transition I calculate the free energies of various mixed phases-different "pasta structures"-in the Wigner-Seitz approximation. Crucially, chirally broken nuclear matter and the approximately chirally symmetric phase (loosely interpreted as quark matter) are treated on the same footing. This allows me to compute the interface profiles of bubbles, rods, and slabs fully consistently, taking into account electromagnetic screening effects and without needing the surface tension as an input. I find that the full numerical results tend to disfavor mixed phases compared to a simple steplike approximation used frequently in the literature and that the predominantly favored pasta structure consists of slabs with a surface tension Σ ≃ 6 MeV=fm 2 .

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“…For vanishing surface tensions and Coulomb interactions, the MP is composed of HM and QM that satisfy the Gibbs condition [1]. If a moderate surface tension is employed, with the charged particles relocate themselves via charge screening effects, geometrical structures appear [6][7][8][9][10][11][12][13][14]. Those structures become unstable for enough large surface tensions, which leads to a bulk separation of quark and hadron phases, i.e., the Maxwell construction scenarios.…”

Section: Introductionmentioning

confidence: 99%

“…In our previous study [13], we considered the possibility of constraining the surface tension from pulsar observations, where a first-order deconfinement phase transition was assumed. By adopting the covariant density functional TW99 [43] for nuclear matter and perturbation model [44] for quark matter, it was found that varying the surface tension value will have sizable effects on the radii and tidal deformabilities of 1.36-solar-mass hybrid stars.…”

Section: Introductionmentioning

confidence: 99%

Systematic study on the quark-hadron mixed phase in compact stars

et al. 2020

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We investigate systematically the quark-hadron mixed phase in dense stellar matter and its influence on compact star structures. The properties of quark matter and hadronic matter are fixed based on various model predictions. Beside adopting constant values, the surface tension Σ for the quark-hadron interface is estimated with the multiple reflection expansion method and equivparticle model. To fix the structures of quark-hadron pasta phases, a continuous dimensionality of the structure is adopted as proposed by Ravenhall et al. The corresponding properties of hybrid stars are then obtained and confronted with pulsar observations. It is found that the correlation between radius and tidal deformability in traditional neutron stars preserves in hybrid stars. For those permitted by pulsar observations, in almost all cases, the quark phase persists inside the most massive compact stars. The quark-hadron interface plays an important role in hybrid star structures once quark matter emerges. The surface tension Σ estimated with various methods increases with density, which predicts stiffer equation of states (EOSs) for the quark-hadron mixed phase and increases the maximum mass of hybrid stars. With or without the emergence of quark matter, the obtained EOSs of hybrid star matter are close to each other at densities n ≲ 0.8 fm −3 , while larger uncertainty is expected at higher densities.

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Constraining quark-hadron interface tension in the multimessenger era

Cited by 33 publications

References 121 publications

Hadron matter in neutron stars in view of gravitational wave observations

Hadron matter in neutron stars in view of gravitational wave observations

Chiral pasta: Mixed phases at the chiral phase transition

Systematic study on the quark-hadron mixed phase in compact stars

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