Constraints on the symmetry energy and its associated parameters from nuclei to neutron stars

Zhang, Yingxun; Liu, Min; Xia, Caichu; Li, Zhuxia; Biswal, S. K.

doi:10.1103/physrevc.101.034303

Cited by 68 publications

(67 citation statements)

References 102 publications

(154 reference statements)

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“…Various studies have empirically identified correlations between various combinations of parameters that characterize the symmetry energy and its density dependence with the neutron star radius and tidal parameters [246,[266][267][268][269] or terrestrial experimental results [239,[270][271][272], as they all are linked to the low-density behavior of the equation of state around (twice) saturation. The tidal constraints from GW170817, and more recently radius constraints from NICER have been used to examine implications for the symmetry energy [273][274][275][276][277][278][279][280][281][282] as well as potential systematics in the mapping [283].…”

Section: Microscopic Propertiesmentioning

confidence: 99%

Neutron-star tidal deformability and equation-of-state constraints

2020

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Despite their long history and astrophysical importance, some of the key properties of neutron stars are still uncertain. The extreme conditions encountered in their interiors, involving matter of uncertain composition at extreme density and isospin asymmetry, uniquely determine the stars' macroscopic properties within General Relativity. Astrophysical constraints on those macroscopic properties, such as neutron star masses and radii, have long been used to understand the microscopic properties of the matter that forms them. In this article we discuss another astrophysically observable macroscopic property of neutron stars that can be used to study their interiors: their tidal deformation. Neutron stars, much like any other extended object with structure, are tidally deformed when under the influence of an external tidal field. In the context of coalescences of neutron stars observed through their gravitational wave emission, this deformation, quantified through a parameter termed the tidal deformability, can be measured. We discuss the role of the tidal deformability in observations of coalescing neutron stars with gravitational waves and how it can be used to probe the internal structure of Nature's most compact matter objects. Perhaps inevitably, a large portion of the discussion will be dictated by GW170817, the most informative confirmed detection of a binary neutron star coalescence with gravitational waves as of the time of writing.

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Section: Microscopic Propertiesmentioning

confidence: 99%

Neutron-star tidal deformability and equation-of-state constraints

2020

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“…[122], while the correlation between the maximum mass M max and Λ 1.4 found in Ref. [89] is not observed due to the first-order deconfinement phase transition.…”

Section: Resultsmentioning

confidence: 75%

“…The corresponding EOSs for hybrid star matter are obtained, which predict the structures of compact stars by solving the TOV equation. It is found that the correlation between radius and tidal deformability in traditional neutron stars [89,122] preserves in hybrid stars. Once quark matter emerges inside compact stars, the quark-hadron interface plays an important role on their structures.…”

Section: Discussionmentioning

confidence: 98%

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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“…Several attempts have been taken to explore this object [40,89]. Some of the suggestions are as follows: (i) It is a heavy NS with deconfined QCD core [90], (ii) a super-fast pulsar [91], (iii) a binary black-hole merger [28,92] and (iv) the DM admixed NS with EOS is sufficiently stiff [40] etc. If this event is the merger of the NS and black hole (NSBH), then the tidal deformability of the NS for the canonical star is Λ 1.4 = 616 +273 −158 .…”

Section: Electric Love Number and Tidal Deformabilitymentioning

confidence: 99%

Dark Matter Effects on the Compact Star Properties

Das

Kumar

et al. 2022

Galaxies

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The neutron star properties are generally determined by the equation of state of β-equilibrated dense matter. In this work, we consider the interaction of fermionic dark matter (DM) particles with nucleons via Higgs exchange and investigate the effect on the neutron star properties with the relativistic mean-field model equation of state coupled with DM. We deduce that DM significantly affects the neutron star properties, such as considerably reducing the maximum mass of the star, which depends on the percentage of the DM considered inside the neutron star. The tidal Love numbers both for electric and magnetic cases and surficial Love numbers are also studied for DM admixed NS. We observed that the magnitude of tidal and surficial Love numbers increases with a greater DM percentage. Further, we present post-Newtonian tidal corrections to gravitational waves decreased by increasing the DM percentage. The DM effect on the GW signal is significant during the late inspiral and merger stages of binary evolution for GW frequencies >500 Hz.

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Constraints on the symmetry energy and its associated parameters from nuclei to neutron stars

Cited by 68 publications

References 102 publications

Neutron-star tidal deformability and equation-of-state constraints

Neutron-star tidal deformability and equation-of-state constraints

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

Dark Matter Effects on the Compact Star Properties

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