Neutron star equation of state: Quark mean-field (QMF) modeling and applications

Li, Ang; Zhu, Zhenyu; Zhou, Enbo; Dong, Jianmin; Hu, Jinniu; Xia, Caichu

doi:10.1016/j.jheap.2020.07.001

Cited by 78 publications

(43 citation statements)

References 135 publications

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“…However, a phase transition was not explicitly taken into account in these previous studies. Although the occurrence of a phase transition in NS cores remains a subject of debate, EOSs with an early phase transition at ∼ 2n 0 (where n 0 = 0.16 fm −3 denotes the nuclear saturation density) are compatible with current NS observations (Al-Mamun et al 2021;Li et al 2020Li et al , 2021Miao et al 2020;Xie & Li 2021). Therefore, there is a possibility that A is a hybrid star with a substantial quark matter core (Li et al 2021).…”

Section: Introductionsupporting

confidence: 54%

On the moment of inertia of PSR J0737-3039 A from LIGO/Virgo and NICER

Miao¹,

Li²

2021

Preprint

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We extend our previous study (Li et al. 2021) on neutron stars with a quark core to predict the moment of inertia of pulsar A in the double pulsar binary J0737-3039, assuming there is a phase transition in the pulsar inner core from the soft QMF or the stiff DD2 hadronic equation of state (EOS) to a high-density phase of quark matter modelled by the generic "constant-sound-speed" (CSS) parameterization. We perform a Bayesian analysis of the moment of inertia by incorporating observational data for the tidal deformability of the GW170817 and GW190425 binary neutron star mergers, as detected by LIGO/Virgo, and the mass and radius of PSR J0030+0451 and MSP J0740+6620, as detected by the Neutron Star Interior Composition Explorer. We find that the most probable values of the moment of inertia of PSR J0737-3039 A are 1.27 +0.18 −0.14 × 10 45 g cm 2 for QMF+CSS and similarly 1.29 +0.26 −0.15 × 10 45 g cm 2 for DD2+CSS at 90% credible interval. We also demonstrate how a moment of inertia measurement would improve our knowledge of the EOS and the mass-radius relation for hybrid stars and discuss whether a quark deconfinement phase transition is supported by the available data and forthcoming data that could be consistent with this hypothesis.

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Section: Introductionsupporting

confidence: 54%

On the moment of inertia of PSR J0737-3039 A from LIGO/Virgo and NICER

Miao¹,

Li²

2021

Preprint

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“…Understanding the nature and constrain the Equation of State (EOS) of dense neutronrich nuclear matter is a major science goal [1][2][3][4] shared by many other astrophysical observations (see, e.g., the analyses and reviews in [5][6][7][8][9][10][11][12][13][14][15][16][17][18][19][20][21]) and terrestrial nuclear experiments (see, e.g., [22][23][24][25][26][27][28][29][30][31][32][33]). However, realizing this goal is very challenging for many scientific and technical reasons.…”

Section: Introductionmentioning

confidence: 99%

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

Cai²,

Wang

et al. 2021

Universe

123

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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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“…Then L W can be estimated to be ∼ 4.0 × 10 48 erg s −1 . Assuming that the rotational inertia of the magnetar is 10 45 g cm 2 and the radius of NS is 10 km (e.g., Li et al 2020), we can obtain that the isotropic energy of plateau E P ∼ F W τ ≃ 2.4 × 10 52 ergs. According to Equations (1) and (3), the effective magnetic field strength on the NS surface B eff and initial period P 0 are calculated, ∼ 5.0 × 10 14 G and ∼ 1.1 ms, respectively.…”

Section: Samplesmentioning

confidence: 99%

Evidence of X-ray plateaus driven by the magnetar spindown winds in gamma-ray burst afterglows

Hou,

Du,

Liu

et al. 2021

Preprint

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The central engine of gamma-ray bursts (GRBs) remains an open and forefront topic in the era of multimessenger astrophysics. The X-ray plateaus appear in some GRB afterglows, which are widely considered to originate from the spindown of magnetars. According to the stable magnetar scenario of GRBs, an X-ray plateau and a decay phase as ∼ t −2 should appear in X-ray afterglows. Meanwhile, the "normal" X-ray afterglow is produced by the external shock from GRB fireball. We analyze the Neil Gehrels Swift GRB data, then find three gold samples, which have an X-ray plateau and a decay phase as ∼ t −2 superimposed on the jet-driven normal component. Based on these features of the lightcurves, we argue that the magnetars should be the central engines of these three GRBs. Future joint multimessenger observations might further test this possibility, then which can be beneficial to constrain GRB physics.

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Neutron star equation of state: Quark mean-field (QMF) modeling and applications

Cited by 78 publications

References 135 publications

On the moment of inertia of PSR J0737-3039 A from LIGO/Virgo and NICER

On the moment of inertia of PSR J0737-3039 A from LIGO/Virgo and NICER

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

Evidence of X-ray plateaus driven by the magnetar spindown winds in gamma-ray burst afterglows

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