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Nuclear Theory·nucl-th

Thursday·September 8, 2022

11 papers—5 primary·6 cross-listed

All11Primary5Cross-lists6
  1. 01

    [Submitted on 6 Sept 2022]

    Comparative study on charge radii and their kinks at magic numbers

    Tomoya Naito · Tomohiro Oishi · Hiroyuki Sagawa · Zhiheng Wang

    Isotope dependences of charge radii, i.e., isotope shifts, calculated by the Skyrme Hartree-Fock, the relativistic mean-field, and the relativistic Hartree-Fock calculations are compared against the experimental data of magic and semimagic nuclei. It is found that the tensor interaction plays a role in reproducing the ``kink'' behavior, irregularity of isotope shifts at the neutron magic number, in the relativistic Hartree-Fock approach. With several Skyrme models, it is found that the kink behavior can be reproduced with the spin-orbit interaction having nonzero isovector channel. The single-particle orbitals near the Fermi energy are crucial to determine the kink size. The effects of the symmetry energy and the pairing interaction are also discussed in relation to the kink behavior.

    Comments:
    22 pages, 34 figures, 10 tables
    Subjects:
    Nuclear Theory (nucl-th); Nuclear Experiment (nucl-ex)
    arXiv:
    2209.02857 [pdf]
    PRC(2023)·35 citations
  2. 02

    [Submitted on 6 Sept 2022]

    Massive neutron stars with small radii in relativistic mean-field models optimized to nuclear ground states

    Tsuyoshi Miyatsu🇰🇷 · Myung-Ki Cheoun🇰🇷 · Kyungsik Kim🇰🇷 · Koichi Saito🇯🇵

    We present an equation of state (EoS) for neutron stars using the relativistic mean-field model with isoscalar- and isovector-meson mixing. Taking into account the results of the neutron skin thickness, , of Pb reported by the PREX collaboration, the dimensionless tidal deformability of a canonical neutron star observed from GW170817, and a compact star implied by the secondary component of GW190814, a new effective interaction is constructed so as to reproduce the saturation condition of nuclear matter and the ground-state properties of finite, closed-shell nuclei. We find that the neutron star EoS exhibits the rapid stiffening around twice the nuclear saturation density, which is caused by the soft nuclear symmetry energy, . It is also noticeable that the thick from the PREX-2 experiment can be achieved with the small slope parameter of stemming from the isoscalar-meson mixing. Thus, we speculate that the secondary component of GW190814 is the heaviest neutron star ever discovered.

    Comments:
    8 pages, 5 figures, 2 tables
    Subjects:
    Nuclear Theory (nucl-th); Nuclear Experiment (nucl-ex)
    arXiv:
    2209.02861 [pdf]
    4 citations
  3. 03

    [Submitted on 7 Sept 2022]

    Strange mesons in nuclei and neutron stars

    Laura Tolos🇪🇸

    The present status in the field of strange mesons in nuclei and neutron stars is reviewed. In particular, the interaction, that is governed by the presence of the , is analyzed and the formation of the bound state is discussed. Moreover, the properties of in dense nuclear matter are studied, in connection with strangeness production in nuclear collisions and kaon condensation in neutron stars.

    Comments:
    6 pages, 1 figure, 1 table, contribution to the proceedings of the 14th International Conference on Hypernuclear and Strange Particle Physics (HYP2022), Prague (Czech Republic), June 27-July 1, 2022
    Subjects:
    Nuclear Theory (nucl-th); High Energy Physics — Experiment (hep-ex); High Energy Physics — Phenomenology (hep-ph)
    arXiv:
    2209.03103 [pdf]
    EPJ Web Conf.(2022)·0 citations
  4. 04

    [Submitted on 7 Sept 2022]

    Free spectator nucleons in ultracentral relativistic heavy-ion collisions as a probe of neutron skin

    Lu-Meng Liu🇨🇳 · Chun-Jian Zhang🇺🇸 · Jun Xu🇨🇳 · Jiangyong Jia🇺🇸 · Guang-Xiong Peng🇨🇳

    Besides the yield ratio of free spectator neutrons produced in ultracentral Zr+Zr to Ru+Ru collisions, we propose that the yield ratio of free spectator neutrons to protons in a single collision system at RHIC and LHC can be a more sensitive probe of the neutron-skin thickness and the slope parameter of the symmetry energy. The idea is demonstrated based on the proton and neutron density distributions of colliding nuclei obtained from Skyrme-Hartree-Fock-Bogolyubov calculations, and a Glauber model that provides information of spectator matter. The final spectator particles are produced from direct emission, clusterization by a minimum spanning tree algorithm or a Wigner function approach, and deexcitation of heavy clusters by GEMINI. A larger associated with a larger value increases the isospin asymmetry of spectator matter and thus leads to a larger , especially in ultracentral collisions where the multiplicity of free nucleons are free from the uncertainties of cluster formation and deexcitation. We have further shown that the double ratio of in isobaric collision systems or in collisions by isotopes helps to cancel the detecting efficiency for protons. Effects from nuclear deformation and electromagnetic excitation are studied, and they are found to be subdominant compared to the expected sensitivity to .

    Comments:
    16 pages, 10 figures
    Subjects:
    Nuclear Theory (nucl-th); High Energy Physics — Experiment (hep-ex); Nuclear Experiment (nucl-ex)
    arXiv:
    2209.03106 [pdf]
    PRC(2022)·26 citations
  5. 05

    [Submitted on 7 Sept 2022]

    Low-energy nuclear physics and global neutron star properties

    Brett V. Carlson🇧🇷 · Mariana Dutra🇧🇷 · Odilon Lourenço🇧🇷 · Jérôme Margueron🇫🇷

    We address the question of the role of low-energy nuclear physics data in constraining neutron star global properties, e.g., masses, radii, angular momentum, and tidal deformability, in the absence of a phase transition in dense matter. To do so, we assess the capacity of 415 relativistic mean field and non-relativistic Skyrme-type interactions to reproduce the ground state binding energies, the charge radii and the giant monopole resonances of a set of spherical nuclei. The interactions are classified according to their ability to describe these characteristics and we show that a tight correlation between the symmetry energy and its slope is obtained providing and nuclei are described with the same accuracy (mainly driven by the charge radius data). By additionally imposing the constraints from isobaric analog states and neutron skin radius in Pb, we obtain the following estimates: MeV and MeV. We then analyze predictions of neutron star properties and we find that the 1.4 neutron star (NS) radius lies between 12 and 14 km for the "better" nuclear interactions. We show that i) the better reproduction of low-energy nuclear physics data by the nuclear models only weakly impacts the global properties of canonical mass neutron stars and ii) the experimental constraint on the symmetry energy is the most effective one for reducing the uncertainties in NS matter. However, since the density region where constraints are required are well above densities in finite nuclei, the largest uncertainty originates from the density dependence of the EDF, which remains largely unknown.

    Comments:
    26 pages, 20 figures
    Subjects:
    Nuclear Theory (nucl-th); High Energy Astrophysical Phenomena (astro-ph.HE)
    arXiv:
    2209.03257 [pdf]
    PRC(2023)·38 citations

Affiliations

first authorsco-authorsvia INSPIRE