Hyperons: the strange ingredients of the nuclear equation of state

Vidaña, Isaac

doi:10.1098/rspa.2018.0145

Cited by 71 publications

(66 citation statements)

References 268 publications

(532 reference statements)

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“…In the core of neutron stars (NS), hyperons coexist in equilibrium with neutrons, protons, and electrons [130][131][132][133]. The decay Λ → na would represent a new cooling mechanism for NS and can thus be constrained by stellar structure calculations and observations.…”

Section: Supernova Boundmentioning

confidence: 99%

“…Our estimates are afflicted by significant uncertainties. Nuclear interactions induce important corrections in the calculation of the number densities [131,133], and there are considerable stellar uncertainties stemming from the complex physics at work in the supernova. Note that the energy loss per unit mass obtained using the approximate formula in Eq.…”

Section: Supernova Boundmentioning

confidence: 99%

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Quark flavor phenomenology of the QCD axion

et al. 2020

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Axion models with generation-dependent Peccei-Quinn charges can lead to flavor-changing neutral currents, thus motivating QCD axion searches at precision flavor experiments. We rigorously derive limits on the most general effective flavor-violating couplings from current measurements and assess their discovery potential. For two-body decays, we use available experimental data to derive limits on q → q 0 a decay rates for all flavor transitions. Axion contributions to neutral-meson mixing are calculated in a systematic way using chiral perturbation theory and operator product expansion. We also discuss in detail baryonic decays and three-body meson decays, which can lead to the best search strategies for some of the couplings. For instance, a strong limit on the Λ → na transition can be derived from the supernova SN 1987A. In the near future, dedicated searches for q → q 0 a decays at ongoing experiments could potentially test Peccei-Quinn breaking scales up to 10 12 GeV at NA62 or KOTO and up to 10 9 GeV at Belle II or BES III.

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Section: Supernova Boundmentioning

confidence: 99%

Section: Supernova Boundmentioning

confidence: 99%

Quark flavor phenomenology of the QCD axion

et al. 2020

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“…where k F = (3π 2 ρ/2) 1/3 is the nucleon Fermi momentum and m * 0 /m = (1 + m 2 kF ∂U 0 /∂k) −1 | kF is the nucleon isoscalar effective mass of nucleons with free mass m. In terms of the m * 0 , the symmetry energy of Eq. (7) can be rewritten as E sym,2 (ρ) = 1 3 k 2 F 2m * 0 (ρ, k F )…”

Section: Decomposition Of the Nuclear Symmetry Energy According To Thmentioning

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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“…The symmetry energy E sym (ρ) at suprasaturation densities and the possible hadronquark phase transition are among the most uncertain parts of the EOS of dense neutronrich matter [12,13,15,29]. Moreover, the appearance of new particles, such as ∆(1232) resonances and various hyperons, also depends strongly on the high-density behavior of nuclear symmetry energy [44][45][46][47][48][49][50][51][52][53][54][55][56][57][58][59]. Since the nuclear symmetry energy will lose its physical meaning above the hadron-quark transition density, it is imperative to determine both the high-density E sym (ρ) and the properties of the hadron-quark phase transition simultaneously by using combined data from astrophysical observations and nuclear experiments.…”

Section: Introductionmentioning

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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Hyperons: the strange ingredients of the nuclear equation of state

Cited by 71 publications

References 268 publications

Quark flavor phenomenology of the QCD axion

Quark flavor phenomenology of the QCD axion

Towards understanding astrophysical effects of nuclear symmetry energy

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

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