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Futoshi Minato (Kyushu university), Kenichi Yoshida (The University of Osaka), Yifei Niu (Lanzhou University)09/09/2025, 16:501. Nuclear structure and reactions
The half-lives of nuclei undergoing $\beta$-decay are highly sensitive to the $Q_{\beta}$ values. In order to achieve reliable theoretical predictions, it is crucial to construct an effective interaction or energy density functional (EDF) capable of systematically reproducing experimental $Q_{\beta}$ values. One of the main challenges is identifying which EDFs can accurately predict...
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Kenta Hagihara (University of Tsukuba)09/09/2025, 16:501. Nuclear structure and reactions
We investigate the role of the Coulomb interaction in nuclear deformation and stability across the nuclear chart. Using self-consistent Hartree-Fock-Bogoliubov (HFB) calculations within DFT theory, we systematically evaluate quadrupole deformation for even-even nuclei with proton numbers ranging from Z=2 to Z=118.
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By comparing results obtained with and without the Coulomb interaction, we find... -
Jeonghyeok Park (Korea Univeristy)09/09/2025, 16:502. Heavy-ion collision experiments and transport model simulations
The triple-differential yield as functions of the transverse momentum, the
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rapidity and the azimuthal angle relative to the estimated reaction plane
is a critical observable for the collective-flow analysis in heavy-ion
collisions. However, the triple-differential yield can be degraded by not
only methodology to estimate reaction plane direction but also imperfect
detector performance... -
Chisato Ruike (University of Tsukuba)09/09/2025, 16:501. Nuclear structure and reactions
One of the important correlations in atomic nuclei is pairing, where two nucleons form a pair. The pairing correlation can lead to a phase transition into a superfluid state, analogous to the superconducting state observed in electronic systems.
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In the superfluid phase, the global U(1) gauge symmetry is spontaneously broken. As a result, a new type of the collective mode emerges: the pair... -
Guilherme Grams (University of Potsdam)09/09/2025, 16:508. Theory of compact stars, including neutron star mergers and supernovae
The properties of neutron star matter in the low-density regime, where nucleonic clusters coexist with a neutron fluid, remain rather uncertain, but are essential for the accurate modelling of neutron star mergers. We systematically explore how nuclear physics inputs, particularly those related to the symmetry energy and the treatment of finite-size effects, impact the properties of warm,...
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Mr Praveen Kumar Yadav (Thapar Institute of Engineering and Technology)09/09/2025, 16:508. Theory of compact stars, including neutron star mergers and supernovae
Neutron stars serve as unique astrophysical laboratories for probing the equation of state (EoS) of matter under extreme density and isospin asymmetry [1]. Understanding their surface characteristics, particularly the surface incompressibility and surface symmetry energy, provides vital constraints on nuclear interactions far from saturation conditions. This study utilizes the coherent density...
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Naibo Zhang (Southeast University)09/09/2025, 16:508. Theory of compact stars, including neutron star mergers and supernovae
By inverting the observational data of several neutron star observables in the three-dimensional parameter space of the constant speed of sound (CSS) model while fixing all hadronic equation-of-state parameters at their currently known most probable values, we constrain the properties of the first-order phase transition from hadronic to quark matter, as well as the speed of sound in quark...
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Takayuki YANO (Kyoto University)09/09/2025, 16:501. Nuclear structure and reactions
Proton elastic scattering is one of the best probes to determine the proton and neutron density distributions in nuclei, which are not only fundamental properties of nuclei but also plays an important role in studying the symmetry energy of the nuclear matter equation of state. We measured the proton elastic scattering from 136Xe at 200 and 300 MeV/nucleon in inverse kinematics with high...
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Dr Akira Dohi (RIKEN)09/09/2025, 16:508. Theory of compact stars, including neutron star mergers and supernovae
The hot neutron star cools down due to the loss of neutrinos produced by the scattering of particles mainly inside the core, which enables us to probe the state of high-density matter through temperature observations. Recent X-ray observations have confirmed the existence of too cold isolated neutron stars beyond the standard cooling scenario without rapid cooling (i.e., minimal cooling...
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Myeong-Hwan Mun (Kyungpook National University)09/09/2025, 16:501. Nuclear structure and reactions
The nuclear symmetry energy is a fundamental component of the nuclear equation of state (EoS) that significantly influences the properties of neutron-rich nuclei, heavy-ion collisions, and neutron star structure. In this study, we employ the deformed relativistic Hartree-Bogoliubov theory in continuum (DRHBc) with the PC-PK1 density functional to systematically investigate the effects of...
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Baiting Tian09/09/2025, 16:504. Isospin and spin dependence of nuclear interactions and correlations
Introduction
The density dependence of nuclear symmetry energy is a key issue in nuclear physics and astrophysics, influencing the structure of neutron stars and the dynamics of supernovae.
The isovector reorientation (IVR) effect in polarized deuteron scattering provides a novel and sensitive probe to constrain the symmetry energy, especially at sub-saturation densities....
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Tomoya Nakada (Kyoto University)09/09/2025, 16:501. Nuclear structure and reactions
The symmetry energy in the equation of state (EoS) of nuclear matter remains one of the key open questions in both nuclear physics and astrophysics, with significant implications for phenomena such as neutron stars and supernova explosions. Our approach focuses on the differences in proton and neutron density distributions among isotopes, which are expected to provide deeper insight into the...
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Mr Dae Ik Kim (Pusan National University)09/09/2025, 16:502. Heavy-ion collision experiments and transport model simulations
The quark-meson coupling (QMC) model incorporates quark degrees of freedom, unlike the quantum hadro-dynamics (QHD) model. Using the mean-field approximation, the QMC model has been applied to nuclear matter, neutron stars, finite nuclei, and related systems. In this work, we investigate heavy-ion collisions by incorporating the QMC model into the Daejeon Boltzmann-Uehling-Ulenbeck (DJBUU)...
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Seon Ho Nam (Korea University)09/09/2025, 16:502. Heavy-ion collision experiments and transport model simulations
The nuclear symmetry energy and its density dependence, particularly
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above saturation density, remain among the most significant
uncertainties in the nuclear equation of state (EoS). These properties
play a crucial role in both intermediate-energy heavy-ion collisions and
the structure of neutron star matter. Experimental information at supra-
saturation densities, however, is still... -
Rongjun Liu (Shanghai Institute of Applied Physics, Chinese Academy of Sciences)09/09/2025, 16:504. Isospin and spin dependence of nuclear interactions and correlations
The dynamical role of the spin-orbit (SO) coupling is a crucial, but not fully understood, aspect in the description of heavy-ion collisions. We investigate this influence using three-dimensional Time-Dependent Hartree-Fock (TDHF) calculations with the SKY3D code. This study simulates heavy-ion collisions ($Z=6-36$, with neutron numbers $N$ from $Z-4$ to $Z+4$) at a center-of-mass kinetic...
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Xuhao Wu09/09/2025, 16:508. Theory of compact stars, including neutron star mergers and supernovae
We examine the effects of symmetry energy on proto-neutron stars (PNSs) using an equation of state
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(EOS) described by the relativistic mean-field (RMF) model. The thermal properties of dense matter and the bulk
properties of PNSs are investigated under the assumptions of isothermy, isentropy, and fixed lepton fractions. The
polytropic index is calculated at finite temperature, revealing a... -
Min Ju (中国石油大学（华东）)09/09/2025, 16:508. Theory of compact stars, including neutron star mergers and supernovae
Neutron stars are considered as the ideal natural laboratories to study the physics of dense matter, where the matter covers a huge range of densities. The baryon number density in the core of the neutron star can reach 5-10 $n_0$ ($n_0 \sim 0.16\ \rm{fm}^{-3}$), so the hadron-quark deconfinement phase transition is likely to occur. Traditionally, the hadron-quark phase transition in neutron...
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