Constraining Neutron Star Matter With Quantum Chromodynamics

Kurkela, Aleksi; Fraga, Eduardo S.; Schaffner-Bielich, J.; Vuorinen, Aleksi

doi:10.1088/0004-637x/789/2/127

Cited by 261 publications

(302 citation statements)

References 26 publications

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“…First principles QCD calculations are not yet able to describe the interactions of such a system at several times the nuclear saturation density (but there is significant recent progress in describing the quark matter EoS at even higher densities and extrapolating down to lower densities; see, e.g., the discussion and results in Kojo et al 2015 andKurkela et al 2014). Because of that, a number of different approaches have been followed in the calculations of the equation of state of neutron star matter.…”

Section: Neutron Star Structurementioning

confidence: 99%

Masses, Radii, and the Equation of State of Neutron Stars

Özel

Freire

2016

Annu. Rev. Astron. Astrophys.

1,389

1,231

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We summarize our current knowledge of neutron star masses and radii. Recent instrumentation and computational advances have resulted in a rapid increase in the discovery rate and precise timing of radio pulsars in binaries in the last few years, leading to a large number of mass measurements. These discoveries show that the neutron star mass distribution is much wider than previously thought, with 3 known pulsars now firmly in the 1.9−2.0 M⊙ mass range. For radii, large, high quality datasets from X-ray satellites as well as significant progress in theoretical modeling led to considerable progress in the measurements, placing them in the 9.9 − 11.2 km range and shrinking their uncertainties due to a better understanding of the sources of systematic errors. The combination of the massive neutron star discoveries, the tighter radius measurements, and improved laboratory constraints of the properties of dense matter has already made a substantial impact on our understanding of the composition and bulk properties of cold nuclear matter at densities higher than that of the atomic nucleus, a major unsolved problem in modern physics.

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Section: Neutron Star Structurementioning

confidence: 99%

Masses, Radii, and the Equation of State of Neutron Stars

Özel

Freire

2016

Annu. Rev. Astron. Astrophys.

1,389

1,231

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“…The resulting pressure versus energy density curve, P (ε), falls well within the acceptable EoS band constrained by neutron star data as discussed in Refs. [115,116,117,118]. Here we briefly examine how this figures in the mass-radius plot for neutron stars, especially in view of the existence of two heavy n-stars with accurately determined masses: J1614-2230 with M = (1.97 ± 0.04) M [119], and J0348+0432 with M = (2.01 ± 0.04) M [120].…”

Section: Constraints From Neutron Starsmentioning

confidence: 99%

Functional renormalization group studies of nuclear and neutron matter

Drews

Weise

2017

Progress in Particle and Nuclear Physics

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Functional renormalization group (FRG) methods applied to calculations of isospinsymmetric and asymmetric nuclear matter as well as neutron matter are reviewed. The approach is based on a chiral Lagrangian expressed in terms of nucleon and meson degrees of freedom as appropriate for the hadronic phase of QCD with spontaneously broken chiral symmetry. Fluctuations beyond mean-field approximation are treated solving Wetterich's FRG flow equations. Nuclear thermodynamics and the nuclear liquid-gas phase transition are investigated in detail, both in symmetric matter and as a function of the proton fraction in asymmetric matter. The equations of state at zero temperature of symmetric nuclear matter and pure neutron matter are found to be in good agreement with advanced ab-initio many-body computations. Contacts with perturbative many-body approaches (in-medium chiral perturbation theory) are discussed. As an interesting test case, the density dependence of the pion mass in the medium is investigated. The question of chiral symmetry restoration in nuclear and neutron matter is addressed. A stabilization of the phase with spontaneously broken chiral symmetry is found to persist up to high baryon densities once fluctuations beyond mean-field are included. Neutron star matter including beta equilibrium is discussed under the aspect of the constraints imposed by the existence of two-solar-mass neutron stars.

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“…Perturbative QCD is valid in the limit of asymptotic freedom where quarks are no longer strongly coupled(cf. Kurkela et al 2014 and references therein). Therefore, it provides a valuable benchmark for the asymptotic behavior of realistic quark matter model EoS.…”

Section: Introductionmentioning

confidence: 99%

Simultaneous Chiral Symmetry Restoration and Deconfinement Consequences for the QCD Phase Diagram

Klähn

Fischer

Hempel

2017

ApJ

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For studies of quark matter in astrophysical scenarios, the thermodynamic bag model is commonly employed. Although successful, it does not account for dynamical chiral symmetry breaking and repulsions due to the vector interaction which is crucial to explain recent observations of massive, two solar mass neutron stars. In Klähn & Fischer we developed the novel vBag quark matter model which takes these effects into account. This article extends vBag to finite temperatures and isospin asymmetry. Another particular feature of vBag is the determination of the deconfinement bag constant B dc from a given hadronic equation of state in order to ensure that chiral and deconfinement transitions coincide. We discuss consequences of this novel approach for the phase transition construction, the phase diagram, and implications for protoneutron stars.

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Constraining Neutron Star Matter With Quantum Chromodynamics

Cited by 261 publications

References 26 publications

Masses, Radii, and the Equation of State of Neutron Stars

Masses, Radii, and the Equation of State of Neutron Stars

Functional renormalization group studies of nuclear and neutron matter

Simultaneous Chiral Symmetry Restoration and Deconfinement Consequences for the QCD Phase Diagram

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