Effects of nuclear symmetry energy on η meson production and its rare decay to the dark U-boson in heavy-ion reactions

Yong, Gao‐Chan; Li, Bao-An

doi:10.1016/j.physletb.2013.05.059

Cited by 22 publications

(13 citation statements)

References 109 publications

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“…The light and weakly interacting U -boson is a favorite candidate mediating the extra interaction [8,35,41], and various new experiments in terrestrial laboratories have been proposed to search for the U -boson, see, e.g., Ref. [42] and references therein. The search for evidence of the modified gravity is at the forefront of research in several sub-fields of natural sciences including geophysics, nuclear and particle physics, as well as astrophysics and cosmology, see, e.g., Refs.…”

Section: Yukawa-type Non-newtonian Gravity and Model Eos Of Hybrimentioning

confidence: 99%

Breaking the EOS-gravity degeneracy with masses and pulsating frequencies of neutron stars

Lin

Chen

et al. 2014

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

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A thorough understanding of many astrophysical phenomena associated with compact objects requires reliable knowledge about both the equation of state (EOS) of super-dense nuclear matter and the theory of strong-field gravity simultaneously because of the EOS-gravity degeneracy. Currently, variations of the neutron star (NS) mass-radius correlation from using alternative gravity theories are much larger than those from changing the NS matter EOS within known constraints. At least two independent observables are required to break the EOS-gravity degeneracy. Using model EOSs for hybrid stars and a Yukawa-type non-Newtonian gravity, we investigate both the mass-radius correlation and pulsating frequencies of NSs. While the maximum mass of NSs increases, the frequencies of the f , p1, p2, and wI pulsating modes are found to decrease with the increasing strength of the Yukawa-type non-Newtonian gravity, providing a useful reference for future determination simultaneously of both the strong-field gravity and the supranuclear EOS by combining data of x-ray and gravitational wave emissions of neutron stars.

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Section: Yukawa-type Non-newtonian Gravity and Model Eos Of Hybrimentioning

confidence: 99%

Breaking the EOS-gravity degeneracy with masses and pulsating frequencies of neutron stars

Lin

Chen

et al. 2014

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

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“…Although significant progress has been made, the symmetry energy is still subject to uncertainties especially at high-density region [11,12]. Nowadays, many sensitive observables have been identified as promising probes of the symmetry energy, such as the π − /π + ratio [13][14][15][16][17][18][19], energetic photon as well as η [20][21][22], the neutron to proton ratio n/p [23][24][25], t/ 3 He [26,27], the isospin fractionation [24,[28][29][30] and the neutron-proton differential flow [31,32]. However, one only knows these observables are in general sensitive to the high-density or low-density behaviors of the symmetry energy at certain beam energy whereas none knows the decomposition of sensitivity of the symmetry energy observables in the whole density region.…”

Section: Introductionmentioning

confidence: 99%

Decomposition of the sensitivity of the symmetry energy observables

2015

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To exactly answer which density region that some frequently used symmetry-energy-sensitive observables probe, for the first time, we make a study of decomposition of the sensitivity of some symmetry-energy-sensitive observables. It is found that for the Au+Au reaction at incident beam energies of 200 and 400 MeV/nucleon, frequently used symmetry-energy-sensitive observables mainly probe the density-dependent symmetry energy around 1.25ρ0 (for pionic observables) or 1.5ρ0 (for nucleonic observables). Effects of the symmetry energy in the low-density region is in general small but observable. The fact that the symmetry-energy-sensitive observables are not sensitive to the symmetry energy in the maximal baryon-density region increases the difficulty of studying nuclear symmetry energy at super-density.

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“…[98]. The decreasing/negative symmetry energy at high densities leads to the interesting possibility of forming proton polarons [99,100] in neutron-rich nucleonic matter, the need for a modified gravity in massive neutron stars [50,51,52] or the existence of a weakly interacting light boson mediating a new force [101,102,103].…”

Section: Tensor Force and High-density Symmetry Energymentioning

confidence: 99%

Origins and impacts of high-density symmetry energy

Li¹

2017

AIP Conference Proceedings

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Abstract. What is nuclear symmetry energy? Why is it important? What do we know about it? Why is it so uncertain especially at high densities? Can the total symmetry energy or its kinetic part be negative? What are the effects of three-body and/or tensor force on symmetry energy? How can we probe the density dependence of nuclear symmetry energy with terrestrial nuclear experiments? What observables of heavy-ion reactions are sensitive to the high-density behavior of nuclear symmetry energy? How does the symmetry energy affect properties of neutron stars, gravitational waves and our understanding about the nature of strong-field gravity? In this lecture, we try to answer these questions as best as we can based on some of our recent work and/or understanding of research done by others. This note summarizes the main points of the lecture.

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Effects of nuclear symmetry energy on η meson production and its rare decay to the dark U-boson in heavy-ion reactions

Cited by 22 publications

References 109 publications

Breaking the EOS-gravity degeneracy with masses and pulsating frequencies of neutron stars

Breaking the EOS-gravity degeneracy with masses and pulsating frequencies of neutron stars

Decomposition of the sensitivity of the symmetry energy observables

Origins and impacts of high-density symmetry energy

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