Erratum: Bounds on the speed of sound in dense matter, and neutron star structure [Phys. Rev. C 
<b>95</b>
, 045801 (2017)]

Moustakidis, Ch. C.; Gaitanos, T.; Margaritis, Ch.; Lalazissis, G. A.

doi:10.1103/physrevc.95.059904

Cited by 29 publications

(20 citation statements)

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“…Fig. 3 also shows that, in our model, the speed of sound never crosses the boundary established by kinetic theory (Moustakidis et al (2017)), c 2 s In addition, for very large densities, our speed of sound remains around √ 1/3, as expected. The pressure of star matter, divided by the Stefan-Boltzmann pressure (ideal-gas limit), as a function of baryo-chemical potential is shown in Fig.…”

Section: Isospin−asymmetric Mattersupporting

confidence: 84%

The application of the Quark-Hadron Chiral Parity-Doublet model to neutron star matter

Mukherjee

Schramm

Steinheimer

et al. 2017

A&A

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Aims. The Quark-Hadron Chiral Parity-Doublet model (QχP) is applied to calculate compact star properties in the presence of a deconfinement phase transition. Methods. Within this model, a consistent description of nuclear matter properties, chiral symmetry restoration, and a transition from hadronic to quark and gluonic degrees of freedom is possible within one unified approach. Results. We find that the equation of state obtained is consistent with recent perturbative quantum chromodynamics (QCD) results and is able to accommodate observational constraints of massive and small neutron stars. Furthermore, we show that important features of the equation of state, such as the symmetry energy and its slope, are well within their observational constraints.Conclusions.

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Section: Isospin−asymmetric Mattersupporting

confidence: 84%

The application of the Quark-Hadron Chiral Parity-Doublet model to neutron star matter

Mukherjee

Schramm

Steinheimer

et al. 2017

A&A

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“…We compare these to the current NS maximummass constraint of 2.01 ± 0.04 M (Antoniadis et al 2013). Depending on the transition density and the nuclear Hamiltonian, we observe the tension between current nuclear and astrophysical constraints and the c 2 S < 1/3 bound set by the conformal limit, first noted in Bedaque & Steiner (2015) (see also Moustakidis et al (2017)). At the lower transition density, there is some freedom to find an EOS that satisfies both the conformal bound and the maximum-mass constraint.…”

Section: Extension With the Conformal Limitmentioning

confidence: 78%

Constraining the Speed of Sound inside Neutron Stars with Chiral Effective Field Theory Interactions and Observations

Tews

Carlson

Gandolfi

et al. 2018

ApJ

402

386

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The dense matter equation of state (EOS) determines neutron star (NS) structure but can be calculated reliably only up to one to two times the nuclear saturation density, using accurate manybody methods that employ nuclear interactions from chiral effective field theory constrained by scattering data. In this work, we use physically motivated ansatzes for the speed of sound c S at high density to extend microscopic calculations of neutron-rich matter to the highest densities encountered in stable NS cores. We show how existing and expected astrophysical constraints on NS masses and radii from X-ray observations can constrain the speed of sound in the NS core. We confirm earlier expectations that c S is likely to violate the conformal limit of c 2 S ≤ c 2 /3, possibly reaching values closer to the speed of light c at a few times the nuclear saturation density, independent of the nuclear Hamiltonian. If QCD obeys the conformal limit, we conclude that the rapid increase of c S required to accommodate a 2 M NS suggests a form of strongly interacting matter where a description in terms of nucleons will be unwieldy, even between one and two times the nuclear saturation density. For typical NSs with masses in the range 1.2 − 1.4 M , we find radii between 10 and 14 km, and the smallest possible radius of a 1.4 M NS consistent with constraints from nuclear physics and observations is 8.4 km. We also discuss how future observations could constrain the EOS and guide theoretical developments in nuclear physics.

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“…The role of speed of sound in dense matter and neutron star properties were stressed recently [21,66,67], and we apply a generic classification of EoSs with regard to their sound-speed behavior as following:…”

Section: Discussionmentioning

confidence: 99%

Tidal deformability with sharp phase transitions in binary neutron stars

2019

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The neutron star tidal deformability is a critical parameter which determines the pre-merger gravitational-wave signal in a neutron star merger. In this article, we show how neutron star tidal deformabilities behave in the presence of one or two sharp phase transition(s). We characterize how the tidal deformability changes when the properties of these phase transitions are modified in dense matter equation of state (EoS). Sharp phase transitions lead to the smallest possible tidal deformabilities and also induce discontinuities in the relation between tidal deformability and gravitational mass. These results are qualitatively unmodified by a modest softening of the phase transition. Finally, we test two universal relations involving the tidal deformability and show that their accuracy is limited by sharp phase transitions. PACS numbers: 97.60.Jd, 95.30.Cq,

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Erratum: Bounds on the speed of sound in dense matter, and neutron star structure [Phys. Rev. C 95 , 045801 (2017)]

Cited by 29 publications

References 0 publications

The application of the Quark-Hadron Chiral Parity-Doublet model to neutron star matter

The application of the Quark-Hadron Chiral Parity-Doublet model to neutron star matter

Constraining the Speed of Sound inside Neutron Stars with Chiral Effective Field Theory Interactions and Observations

Tidal deformability with sharp phase transitions in binary neutron stars

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