Investigating effects of relativistic kinematics, dimensionality, interactions, and short-range correlations on the ratio of quartic over quadratic nuclear symmetry energies

Cai, Bao-Jun; Li, Bao-An

doi:10.1103/physrevc.105.064607

Cited by 7 publications

(5 citation statements)

References 54 publications

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“…(d) In this work, we study the EOS of ANM in a space of general dimension d totally adopting the nonrelativistic calculations. Since the relativistic kinematics, the nucleon-nucleon interactions, and/or the dimensionality together may effectively affect the EOS of ANM [100], it would be extremely interesting to marry the relativistic kinematics and the fruitful nucleon-nucleon interactions (we have already found that the momentum dependence of the single-nucleon potential could effectively influence certain problems) in the general dimension d and to explore how they influence each other coherently. See the following overall scheme (see (2.21) for the definition of θ f and e J is the general relativistic single-nucleon energy [63]) on its inner relations.…”

Section: Summary and Discussion Of Some Unresolved Issues For Future ...mentioning

confidence: 99%

“…The single-nucleon energy in dD still reads e J (ρ,δ,|k|) = k 2 /2M + U J (ρ,δ,|k|), with the first term the kinetic energy and the second term the potential energy. Considering the free Fermi gas (FFG) model, we have for the kinetic part of the EOS as [100],…”

Section: Generalization To Dd Spacementioning

confidence: 99%

“…In the infinite-d limit, we have then E sym (ρ 0 )/E sym,4 (ρ 0 ) = U sym,3 /2U sym ≪ 1. Writing out the EOS of ANM in a general dimension d thus gives us extra insight into the strength of different expansion terms, and from this viewpoint, the goodness of the conventional parabolic approximation in 3D has no magic origin [100].…”

Section: The Two-dimensional Nucleonic Eosmentioning

confidence: 99%

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Equation of State of Neutron-Rich Matter in $d$-Dimensions

Cai¹,

Li²

2022

Preprint

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Nuclear systems under constraints, with high degrees of symmetries and/or collectivities may be considered as moving effectively in spaces with reduced spatial dimensions. We first derive analytical expressions for the nucleon specific energy E 0 (ρ), pressure P 0 (ρ), incompressibility coefficient K 0 (ρ) and skewness coefficient J 0 (ρ) of symmetric nucleonic matter (SNM), the quadratic symmetry energy E sym (ρ), its slope parameter L(ρ) and curvature coefficient K sym (ρ) as well as the fourth-order symmetry energy E sym,4 (ρ) of neutron-rich matter in general d spatial dimensions (abbreviated as "dD") in terms of the isoscalar and isovector parts of the isospin-dependent single-nucleon potential according to the generalized Hugenholtz-Van Hove (HVH) theorem. The equation of state (EOS) of nuclear matter in dD can be linked to that in the conventional 3-dimensional (3D) space by the ǫ-expansion which is a perturbative approch successfully used previously in treating second-order phase transitions and related critical phenomena in solid state physics and more recently in studying the EOS of cold atoms. The ǫ-expansion of nuclear EOS in dD based on a reference dimension d f = d − ǫ is shown to be effective with −1 ǫ 1 starting from 1 d f 3 in comparison with the exact expressions derived using the HVH theorem. Moreover, the EOS of SNM (with/without considering its potential part) is found to be reduced (enhanced) in lower (higher) dimensions, indicating in particular that the many-nucleon system tends to be deeper bounded but saturate at higher densities in spaces with lower dimensions. The symmetry energy perturbed from its counterpart in 3D is found to strongly depend on the momentum-dependence of the nucleon isovector potential. Moreover, the specific structure of the fourth-order symmetry energy in dD is also analyzed generally, and it is found to be naturally small, confirming the parabolic approximation for the EOS of neutron-rich matter from an even wider viewpoint. The links between the EOSs in 3D and dD spaces from the ǫ-expansion provide new perspectives to the EOS of neutron-rich matter. Further studies and potential applications of these links in nuclear physics and/or astrophysics are discussed.

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Section: Summary and Discussion Of Some Unresolved Issues For Future ...mentioning

confidence: 99%

Section: Generalization To Dd Spacementioning

confidence: 99%

Section: The Two-dimensional Nucleonic Eosmentioning

confidence: 99%

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Equation of State of Neutron-Rich Matter in $d$-Dimensions

Cai¹,

Li²

2022

Preprint

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“…Interesting indications have been found very recently of SRC effects on the cooling of protoneutron stars, the formation of baryon resonances, dark matter, and nuclear pasta as well as on tidal deformation and mass-radius correlation in neutron stars [680][681][682][683][684][685][686][687], and also on several features of nuclear matter and heavy-ion reactions [688][689][690][691][692][693][694][695]. However, much more work remains to be done to systematically and consistently address the SRC-related issues in hadronic transport simulations (see Section II A).…”

Section: B Nuclear Eos With Reduced Spatial Dimensionsmentioning

confidence: 99%

Dense Nuclear Matter Equation of State from Heavy-Ion Collisions

Sorensen¹,

Agarwal²,

Brown³

et al. 2023

Preprint

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“…Other type of interactions between DM and observable matter are also possible, since some upper limits are verified. In particular, in Lourenço et al (2022a,b) the lightest neutralino with mass of = 200 GeV was used as dark particle coupled through the Higgs boson to nucleons presenting short-range correlations (SRC) (Hen et al 2014;CLAS Collaboration 2018Schmidt et al 2020;Hen et al 2017;Duer et al 2019;Li et al 2008;Cai & Li 2016;Guo et al 2021;Cai & Li 2022;Souza et al 2020). Such correlations are experimentally verified in electroninduced quasielastic proton knockout reactions, in which nucleons correlate in pairs with high relative momentum.…”

Section: Introductionmentioning

confidence: 99%

Dark particle mass effects on neutron star properties from a short-range correlated hadronic model

Dutra

Lenzi

Lourenço

2022

Monthly Notices of the Royal Astronomical Society

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In this work we study a relativistic mean-field (RMF) hadronic model, with nucleonic short-range correlations (SRC) included, coupled to dark matter (DM) through the Higgs boson. We study different parametrizations of this model by running the dark particle Fermi momentum, and its mass in the range of 50GeV ≤ Mχ ≤ 500GeV, compatible with experimental spin-independent scattering cross-sections. By using this RMF-SRC-DM model, we calculate some neutron star quantities, namely, mass-radius profiles, dimensionless tidal deformabilities, and crustal properties. Our findings show that is possible to construct RMF-SRC-DM parametrizations in agreement with constraints provided by LIGO and Virgo collaboration (LVC) on the GW170817 event, and recent observational data from the NICER mission. Furthermore, we show that the increase of Mχ favors the model to attain data from LVC regarding the tidal deformabilities. Higher values of Mχ also induce a reduction of the neutron star crust (mass and thickness), and cause a decrease of the crustal fraction of the moment of inertia (Icrust/I). Nevertheless, we show that some RMF-SRC-DM parametrizations still exhibit $I_{\mbox{crust}}/I>7\%$, a condition that explains the glitch activity in rotation-powered pulsars such as the Vela one. Therefore, dark matter content can also be used for describing such a phenomenon.

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Investigating effects of relativistic kinematics, dimensionality, interactions, and short-range correlations on the ratio of quartic over quadratic nuclear symmetry energies

Cited by 7 publications

References 54 publications

Equation of State of Neutron-Rich Matter in $d$-Dimensions

Equation of State of Neutron-Rich Matter in $d$-Dimensions

Dense Nuclear Matter Equation of State from Heavy-Ion Collisions

Dark particle mass effects on neutron star properties from a short-range correlated hadronic model

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