Neutron Star Equation of State from the Quark Level in Light of GW170817

Zhu, Zhenyu; Zhou, Enbo; Li, Ang

doi:10.3847/1538-4357/aacc28

Cited by 118 publications

(110 citation statements)

References 92 publications

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“…[124][125][126][127] The slope parameter for the present model (L 0 = 87 MeV), although a bit larger than that suggested by, 128 is within the range L 0 = (25 − 115) MeV as suggested by. 129 Moreover, recently 8,130 have shown from the co-relation between Table 1. Parameter set of the nuclear matter model considered for the present work (adopted from 30,31,49,63 ).…”

Section: The Model Parametermentioning

confidence: 99%

Role of Δs in determining the properties of neutron stars in parameterized hydrostatic equilibrium

Sen

2019

Int. J. Mod. Phys. D

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The possible existence of [Formula: see text] resonances is inspected in the cold dense matter of neutron star (NS) core in the presence of hyperons. The diverse effects of variation in [Formula: see text] mass on their formation and the equation of state (EoS) are studied in this work with an effective chiral model and the resultant NS properties are calculated with the help of parameterized Tolman–Oppenheimer–Volkoff (PTOV) equations to bring out the two important features of pressure in the context of massive NSs. The [Formula: see text] puzzle is re-explored and resolved taking into account the concept of modified/parametrized inertial pressure and self-gravity in case of massive pulsars like PSR J1614−2230 and PSR J0348-0432. It is seen that although the presence of exotic matter like the hyperons and [Formula: see text] softens the EoS considerably, their presence in massive NSs can be successfully explained with the theory of parametrized hydrostatic equilibrium conditions. The results of this work also satisfy the constraints on [Formula: see text] and [Formula: see text] from the gravitational wave (GW170817) detection of binary NS merger. The constraint on baryonic mass from PSR J0737-3039 is also satisfied with the solutions of the PTOV equations for all the [Formula: see text] masses considered.

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Section: The Model Parametermentioning

confidence: 99%

Role of Δs in determining the properties of neutron stars in parameterized hydrostatic equilibrium

Sen

2019

Int. J. Mod. Phys. D

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“…On the other hand, it has already been pointed out in the literature and discussed in detail in Sect. 5.3.1 that translating Λ measurements directly into R constraints has to be taken with caution [387], and that both Λ and R must be measured independently [120,268] to extract meaningful constraints on the EOS of dense neutron-rich matter. Thus, theoretical predictions of the neutron-star moment of inertia are very timely and important in the ongoing efforts to determine the exact details of the EOS.…”

Section: Symmetry Energy Effects On the Moment Of Inertia Of Slowly Rmentioning

confidence: 99%

Towards understanding astrophysical effects of nuclear symmetry energy

et al. 2019

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Determining the Equation of State (EOS) of dense neutron-rich nuclear matter is a shared goal of both nuclear physics and astrophysics. Except possible phase transitions, the density dependence of nuclear symmetry Esym(ρ) is the most uncertain part of the EOS of neutron-rich nucleonic matter especially at supra-saturation densities. Much progresses have been made in recent years in predicting the symmetry energy and understanding why it is still very uncertain using various microscopic nuclear many-body theories and phenomenological models. Simultaneously, significant progresses have also been made in probing the symmetry energy in both terrestrial nuclear laboratories and astrophysical observatories. In light of the GW170817 event as well as ongoing or planned nuclear experiments and astrophysical observations probing the EOS of dense neutron-rich matter, we review recent progresses and identify new challenges to the best knowledge we have on several selected topics critical for understanding astrophysical effects of the nuclear symmetry energy.PACS. 2 6.60.Kp Contents B.A Li, P.G. Krastev, D.H. Wen and N.B. Zhang: Astrophysical Effects of Nuclear Symmetry Energy 5.2.2 Predicted correlation strength between the radii of neutron stars and the symmetry energy from low to high densities 32 5.2.3 Predicted effects of the symmetry energy on the tidal deformability of neutron stars 33 5.3 Post-GW170817 analyses of tidal deformability and radii of neutron stars as well as constraints on the nuclear EOS and symmetry energy . . . 34 5.3.

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“…Thus, the often used practice of labeling predicted E sym (ρ) with L alone and comparing the corresponding R 1.4 and Λ 1.4 is insufficient. Indeed, "there is no evidence for a simple relation between the symmetry energy slope L (hence the radius) and the tidal deformability [16]." Moreover, by definition, the K sym reflects the change of L. The possible observation of a stiffer E sym (ρ) at sub-saturation densities from terrestrial experiments, such as the sizes of neutron skins of heavy nuclei, and a softer E sym (ρ) at supra-saturation densities from NS radius or tidal polarizability measurements is not necessarily an indication of any phase transition.…”

Section: Inferring the Density Dependence Of Nuclear Symmetry Energy mentioning

confidence: 99%

Delineating effects of nuclear symmetry energy on the radii and tidal polarizabilities of neutron stars

Zhang

2018

J. Phys. G: Nucl. Part. Phys.

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What can we learn about the density dependence of nuclear symmetry energy E sym (ρ) from precise measurements of the radius (R 1.4 ) and/or tidal polarizability (Λ 1.4 ) of canonical neutron stars (NSs) with a mass of 1.4 M ⊙ ? With the E sym (ρ) parameterized using three parameters L, K sym , and J sym which have the asymptotic meaning of being respectively the slope, curvature, and skewness of symmetry energy at saturation density, we found that, while both the R 1.4 and Λ 1.4 depend strongly on the slope L, the K sym and J sym parameters characterizing the high-density behavior of E sym (ρ) also play appreciable roles. Thus, there is not a simple relation between the Λ 1.4 /R 1.4 and L alone. Precise measurements of just the Λ 1.4 and R 1.4 can not completely determine the E sym (ρ) but limit combinations of its parameters. In particular, stringent constraints approximately independent of the J sym on the L-K sym correlations can be obtained. However, infinite combinations of the larger (smaller) L and smaller (larger) K sym can lead to the same Λ 1.4 and R 1.4 . Additional observables including those from terrestrial nuclear experiments are thus necessary to break this degeneracy in order to completely determine the density dependence of nuclear symmetry energy E sym (ρ).

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Neutron Star Equation of State from the Quark Level in Light of GW170817

Cited by 118 publications

References 92 publications

Role of Δs in determining the properties of neutron stars in parameterized hydrostatic equilibrium

Role of Δs in determining the properties of neutron stars in parameterized hydrostatic equilibrium

Towards understanding astrophysical effects of nuclear symmetry energy

Delineating effects of nuclear symmetry energy on the radii and tidal polarizabilities of neutron stars

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