Future prospects for constraining nuclear matter parameters with gravitational waves

Carson, Zack; Steiner, Andrew W.; Yagi, Kent

doi:10.1103/physrevd.100.023012

Cited by 32 publications

(22 citation statements)

References 73 publications

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“…More specifically, (1) and (2) were from Malik et al [64] and (3), (4), and (5) from Biswas et al [65]. The rest were from (6) Zimmerman et al [88], (7) Tsang et al [66], (8) Xie and Li [67], (9) Baillot d'Etivaux et al [68], (10) Malik et al [69], (11) Lim and Holt [71], (12) Chamel et al [75], (13) Raithel and Özel [79], (14) Carson et al [89], (15) Yue et al [80], and (16) Essick et al [81]. The average of these 16 new analyses was about K sym ≈ −107 ± 88 MeV at a 68% confidence level.…”

Section: Updated Systematics Of Symmetry Energy Parameters At ρ 0 After Incorporating the Results Of Recent Analyses Of Neutron Star Obsementioning

confidence: 99%

Progress in Constraining Nuclear Symmetry Energy Using Neutron Star Observables Since GW170817

Cai²,

Wang

et al. 2021

Universe

146

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The density dependence of nuclear symmetry energy is among the most uncertain parts of the Equation of State (EOS) of dense neutron-rich nuclear matter. It is currently poorly known especially at suprasaturation densities partially because of our poor knowledge about isovector nuclear interactions at short distances. Because of its broad impacts on many interesting issues, pinning down the density dependence of nuclear symmetry energy has been a longstanding and shared goal of both astrophysics and nuclear physics. New observational data of neutron stars including their masses, radii, and tidal deformations since GW170817 have helped improve our knowledge about nuclear symmetry energy, especially at high densities. Based on various model analyses of these new data by many people in the nuclear astrophysics community, while our brief review might be incomplete and biased unintentionally, we learned in particular the following: (1) The slope parameter L of nuclear symmetry energy at saturation density ρ0 of nuclear matter from 24 new analyses of neutron star observables was about L≈57.7±19 MeV at a 68% confidence level, consistent with its fiducial value from surveys of over 50 earlier analyses of both terrestrial and astrophysical data within error bars. (2) The curvature Ksym of nuclear symmetry energy at ρ0 from 16 new analyses of neutron star observables was about Ksym≈−107±88 MeV at a 68% confidence level, in very good agreement with the systematics of earlier analyses. (3) The magnitude of nuclear symmetry energy at 2ρ0, i.e., Esym(2ρ0)≈51±13 MeV at a 68% confidence level, was extracted from nine new analyses of neutron star observables, consistent with the results from earlier analyses of heavy-ion reactions and the latest predictions of the state-of-the-art nuclear many-body theories. (4) While the available data from canonical neutron stars did not provide tight constraints on nuclear symmetry energy at densities above about 2ρ0, the lower radius boundary R2.01=12.2 km from NICER’s very recent observation of PSR J0740+6620 of mass 2.08±0.07M⊙ and radius R=12.2–16.3 km at a 68% confidence level set a tight lower limit for nuclear symmetry energy at densities above 2ρ0. (5) Bayesian inferences of nuclear symmetry energy using models encapsulating a first-order hadron–quark phase transition from observables of canonical neutron stars indicated that the phase transition shifted appreciably both L and Ksym to higher values, but with larger uncertainties compared to analyses assuming no such phase transition. (6) The high-density behavior of nuclear symmetry energy significantly affected the minimum frequency necessary to rotationally support GW190814’s secondary component of mass (2.50–2.67) M⊙ as the fastest and most massive pulsar discovered so far. Overall, thanks to the hard work of many people in the astrophysics and nuclear physics community, new data of neutron star observations since the discovery of GW170817 have significantly enriched our knowledge about the symmetry energy of dense neutron-rich nuclear matter.

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Section: Updated Systematics Of Symmetry Energy Parameters At ρ 0 After Incorporating the Results Of Recent Analyses Of Neutron Star Obsementioning

confidence: 99%

Progress in Constraining Nuclear Symmetry Energy Using Neutron Star Observables Since GW170817

Cai²,

Wang

et al. 2021

Universe

146

View full text Add to dashboard Cite

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“…This observation clearly reject the NL3 and IU-FSU phenomenological model in determining the NM parameters for astrophysical observations and hints for G3 EoS, best suited for the study of astrophysical phenomena. Studies show that there is a strong correlation between K sym,0 , tidal deformability and R 1.4 (radius of NS with mass 1.4 M ) [63][64][65]. By obligating K sym,0 in the befitting range we can measure tidal deformability theoretically, which is quite a complicated quantity to measure independently, precisely upto a certain level of accuracy.…”

Section: Resultsmentioning

confidence: 99%

Warm dense matter and cooling of supernovae remnants

et al. 2020

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We study the thermal effects on the nuclear matter (NM) properties such as binding energy, incompressibility, free symmetry energy and its coefficients using NL3, G3 and IU-FSU parameter sets of relativistic mean-field models. These models being consistent with the properties of cold NM, have also been used to study the effect of temperature by incorporating the Fermi function. The critical temperature for the liquid-gas phase transition in the symmetric NM is found to be 14.60, 15.37 and 14.50 MeV for NL3, G3 and IU-FSU parameter sets respectively, which is in excellent agreement with previous theoretical and experimental studies. We inspect that the properties related to second differential coefficient of the binding energy and free symmetry energy at saturation density ( i.e. $$K_{0}(n,T)$$K0(n,T) and $$Q_{sym,0}$$Qsym,0 ) exhibit the contrary effects for NL3 and G3 parameters as the temperature increases. We find that the prediction of saturated curvature parameter ( $$K_{sym,0}$$Ksym,0 ) for G3 equation of state at finite temperature favour the combined analysis of $$K_{sym,0}$$Ksym,0 for the existence of massive pulsars, gravitational waves from GW170817 and NICER observations of PSR J0030+0451. Further, we investigate the cooling mechanism of newly born stars through neutrino emissivity controlled by direct Urca process and instate some interesting remarks about neutrino emissivity. We also deliberate the effect of temperature on the M-R profile of Proto-Neutron star.

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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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Future prospects for constraining nuclear matter parameters with gravitational waves

Abstract: 1 Piecewise polytropic constructions [19-21] and spectral EoSs [8, 22-25] similarly parameterize nuclear matter EoSs in a modelindependent way. See also [12, 26] for related works on piecewise unified EoSs. arXiv:1906.05978v2 [gr-qc]

Cited by 32 publications

References 73 publications

Progress in Constraining Nuclear Symmetry Energy Using Neutron Star Observables Since GW170817

Progress in Constraining Nuclear Symmetry Energy Using Neutron Star Observables Since GW170817

Warm dense matter and cooling of supernovae remnants

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

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