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29/04/2026, 09:30
Atsushi Hosaka
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Yongfeng Huang (Nanjing University)29/04/2026, 09:40
Strange-quark matter (SQM) may be the true ground state of hadronic matter, indicating that the observed pulsars may actually be strange stars (SSs), but not neutron stars. According to the SQM hypothesis, the existence of a hydrostatically stable sequence of SQM stars has been predicted, ranging from 1 to 2 solar mass SSs, to smaller strange dwarfs and even strange planets. While...
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He Gao29/04/2026, 10:15
The increasing number of compact binary coalescences observed by the LIGO-Virgo-KAGRA (LVK) Collaboration, highlighted by the landmark multimessenger detection of the binary neutron star merger GW170817, has opened new frontiers in nuclear astrophysics. This report presents a methodology to constrain the maximum mass of neutron stars, and consequently the neutron star equation of state, by...
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Zhiqiang Miao (Tsung-Dao Lee Institute)29/04/2026, 10:50
We identify a previously unrecognized spin–orbit resonance that can naturally arise in neutron star binaries. This resonance provides a new and direct probe of neutron star ellipticity, enabled by finite stellar quadrupole moments such as those produced by strong internal magnetic fields. We show that the resonance produces a distinctive and measurable gravitational-wave phase shift, allowing...
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Anagh Venneti (Department of Physics, Birla Institute of Technology and Sciences Pilani, Hyderabad campus)29/04/2026, 11:40
The internal composition of compact stars remains largely unresolved in spite of the latest mass–radius measurements by NICER and tidal deformability constraints from gravitational-wave observations. A central challenge is to identify the distinction in the macroscopic observable structure of nucleonic neutron stars and self-bound quark stars. We employ a leave-one-out cross-validation...
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Gihwan Nam (Yonsei)29/04/2026, 12:00
We obtain a empirical relation for the neutron star maximum mass arising from a particular
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combination of the saturation density (n0), the effective mass (m∗), and (when present) the vector
meson self-coupling constant (ζ) within the relativistic mean-field model framework. Observations
of massive neutron stars heavier than ∼ 2M⊙ have eliminated the softest equation of state... -
Ulugbek Yakhshiev (Inha University)29/04/2026, 12:20
We discuss the properties of the static neutron stars and strangeness-mixed stars, based on the equations of state derived from a pion mean-field approach. The model parameters are fixed according to the phenomenological observation related to the pion-nucleus scattering and the bulk properties of nuclear matter near the saturation point. We examine the energy and pressure behavior inside a...
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Myeong-Hwan Mun (Kyungpook National University)29/04/2026, 13:40
Understanding dense and hot QCD matter in compact stars, supernovae, and neutron-star mergers requires reliable microscopic nuclear physics inputs far from the valley of stability. Nuclear mass tables provide essential quantities such as binding energies, neutron separation energies, β-decay Q-values, and nuclear deformation, which directly affect the equation of state, r-process...
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Lap-Ming Lin (The Chinese University of Hong Kong)29/04/2026, 14:15
The trace anomaly $\Delta$ is an important quantity that measures the broken conformal symmetry in neutron star matter. In this talk, we will introduce quasi-universal relations that connect the stellar profile of $\Delta$ to the compactness, moment of inertia, and tidal deformability of neutron stars. We will also discuss how the behavior of $\Delta$ inside neutron stars can be inferred from...
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Masayasu Harada (KMI, Nagoya University)29/04/2026, 15:20
I will briefly summarize our works in which we studied neutron star property based on Parity Doublet Models. In the low-density region, we construct the EoS using hadronic models based on the parity doublet structure with the chiral invariant mass of nucleons. In the high density region, the EoS is obtained in an NJL-type quark model. By connecting two EoSs with assuming the quark-hadron...
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Bikai Gao (RCNP, Osaka University)29/04/2026, 15:55
The ``hyperon puzzle'' remains a fundamental challenge in nuclear astrophysics. We investigate hyperon emergence in neutron star matter using the $SU(3)$ parity doublet model with chiral representation $(3,\bar{3}) + (\bar{3},3)$. This framework naturally incorporates chiral symmetry restoration and provides a systematic description of baryon masses in dense matter through the interplay...
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Luca Passarella (Politecnico di Torino and INFN)29/04/2026, 16:15
We present an equation of state for strongly interacting matter applicable over a broad range of temperatures and baryon densities. This is based on an effective Lagrangian with explicitly broken chiral symmetry, where scale-invariance breaking is regulated by a dilaton field that mimics the dynamics of the gluon condensate in quantum chromodynamics (QCD). The model includes baryons and mesons...
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Jing- Jing Geng (Yangzhou University)29/04/2026, 16:35
Abstract
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Bayesian analysis methodologies provide a robust framework for systematically integrating prior knowledge to refine the understanding of parameter spaces in theoretical models. Consequently, this approach has emerged as a pivotal tool in research domains such as nuclear physics and nuclear astrophysics. Leveraging experimental data from finite nuclei, we employ Bayesian analysis to... -
Tsuneo NODA (Kurume Institute of Technology)29/04/2026, 16:35
Neutron stars are compact objects that can be likened to a single gigantic nucleus. Their central density exceeds nuclear density, allowing diverse states to appear that are not seen in ordinary nuclei, such as hyperon mixing, quark deconfinement and nucleon superfluidity. These states strongly affect the neutrino emission dominating neutron star cooling, thereby determining their thermal...
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Kanji Mori (Keio University)29/04/2026, 16:35
Recent studies on the dark photon (DP) production in collapsing stars argue that the cooling effect induced by DPs can hinder supernova explosions and lead to a ``failing supernova" constraint on the photon-DP mixing parameter $\epsilon$. In order to verify the idea, we perform two-dimensional neutrino-radiation hydrodynamic simulations coupled with the DP production with the masses of 0.3 and...
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Takumi Muto (千葉工業大学)29/04/2026, 16:35
We consider a response of kaon-condensed phase in hyperon-mixed matter [(Y+K) phase] to neutron-star oscillations. We obtain the sound velocity propagating in the (Y+K) phase out of chemical equilibrium with respect to the relevant weak reactions, searching for signals unique to kaon condensation associated with typical gravitational wave modes. The dissipation of vibrational energy including...
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Tatsuya Matsuki (Tokyo University of Science)29/04/2026, 16:35
This study focuses on constructing equations of state based on relativistic mean-field (RMF) theory to investigate the impact of remaining uncertainties in nuclear matter properties. We examine two key factors: the nucleon effective mass and the presence of multineutron states in non-uniform nuclear matter.
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Our results demonstrate that a larger nucleon effective mass within the RMF enhances... -
Xuhao Wu29/04/2026, 16:35
Title: Impact of Hexaquark H Particle on Compact Star Properties
Abstract： We study the possible existence of the hexaquark H particle (uuddss) in neutron stars. Within the Chromomagnetic Interaction framework, the flavor-singlet H exhibits a mass of 2212.7 MeV. Using the relativistic mean-field model, we explore how H particle couplings influence neutron star structure. Our results...
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Ken'ichiro Nakazato29/04/2026, 16:35
The cooling of protoneutron stars (PNSs) via neutrino emission and the onset of crust formation are both governed by the nuclear equation of state (EOS). In particular, properties of dense matter affect not only the neutrino opacity and thermal evolution, but also the characteristics of heavy nuclei emerging in the outer layers. This suggests a nontrivial interplay between neutrino cooling and...
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Hajime SOTANI (Kochi University)29/04/2026, 16:35
By identifying quasi-periodic oscillations reported in FRB 20240114A (from the Five-hundred-meter Aperture Spherical Telescope) with neutron star crustal torsional oscillations, together with experimental constraints on the nuclear saturation parameter, the incompressibility, we constrain the mass and radius of an extragalactic neutron star at redshift z=0.13. Identifying the low-order QPO...
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Davood Rafiei Karkevandi29/04/2026, 16:35
In this talk, I will discuss the effects of self-interacting bosonic dark matter on neutron stars in light of recent observations from NICER and LIGO/Virgo. In this framework, sub-GeV bosonic dark matter can be present either as a dense core inside the star or as an extended halo around it, modifying key observable properties such as the mass, radius, and tidal deformability. By varying the...
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Mamiya Kawaguchi (Anhui University of Science and Technology)29/04/2026, 16:35
The nucleon mass consists of a chiral-variant part and a chiral-invariant part. This mass decomposition is essential for understanding the properties of dense nuclear matter, especially in the high-density region across the chiral phase transition. While the value of the chiral-invariant mass significantly influences the equation of state of neutron stars, its magnitude remains poorly...
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Mahboubeh Shahrbaf Motlagh (University of Wroclaw)29/04/2026, 16:35
The possible presence of dark matter in neutron star interiors may significantly affect their structure and observable properties. Among various candidates, the hypothetical sexaquark has been proposed as a bosonic dark matter particle that could form under the extreme conditions of neutron star cores. In this work, we investigate whether a hybrid neutron star model including hyperons, bosonic...
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Masayuki Kanazawa (Nagoya University)29/04/2026, 16:35
The baryon mass originates from spontaneous chiral symmetry breaking and a chiral invariant mass. The chiral invariant mass of hyperons has not been sufficiently considered. In this study, we investigate the dependence of the density at which hyperons appear on their chiral invariant masses in neutron star matter. We employ SU(2)L×SU(2)R chiral symmetry and introduce the chiral invariant...
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Yuk-Kei Kong (Nagoya University)29/04/2026, 16:35
The properties of dense, neutron-rich matter are strongly influenced by the isovector structure of the nuclear interaction. In particular, the isovector scalar meson a0(980) (also known as the delta meson) modifies the neutron–proton effective mass splitting and significantly affects the behavior of isospin-asymmetric matter. In this talk, we construct an extended parity doublet model...
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Toshiki Maruyama (JAEA)29/04/2026, 16:35
We formulate molecular dynamics for spin systems by time-dependent SU(2) spinor parametrized with two real angles. With central interaction between particles, the total angular momentum and the total spin are conserved as well as the total energy and momentum.But with inclusion of spin-orbit interaction the total angular momentum and total spin become time-dependent quantity. They convert to...
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Wen-Li Yuan (Peking University)29/04/2026, 16:35
We investigate the stability of beta-equilibrated three-flavor color-superconducting quark matter within the Nambu–Jona–Lasinio model under conditions relevant to compact stars. Owing to the attractive interaction between quarks, color superconductivity is expected to occur, with the color–flavor-locked phase favored at high densities. Motivated by the observations of possible low-mass...
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Kohsuke Sumiyoshi (National Institute of Technology, Numazu College)30/04/2026, 09:00
I will provide an overview of the role of hot, dense matter in core-collapse supernovae and neutron stars, with a particular focus on the crucial roles of neutrinos. Supernovae, which result from the gravitational collapse of massive stars, produce bright optical displays, compact objects (such as neutron stars or black holes), and intense bursts of neutrinos. The explosion mechanism remains...
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34. Modeling of binary neutron star mergers for multi-messenger inference of neutron star propertiesSho Fujibayashi (Tohoku University)30/04/2026, 09:35
The gravitational waves emitted by a binary of two neutron stars tell us not only information about the mass of neutron stars, but also information about the matter properties of deep inside neutron stars. The electromagnetic waves emitted by matter expelled by several mechanisms after the merger reveal the binary's post-merger activity. By combining those two 'messengers', we can better...
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Yongjia Huang (Purple Mountain Observatory / RIKEN)30/04/2026, 10:10
The convergence of multi-messenger observations—NICER, GW170817, and theoretical calculations—has tightly constrained the neutron star equation of state, pointing to a non-monotonic sound speed that suggests possible quark matter in massive neutron star cores. However, the masquerade effect obscures the nature of this transition in static stars.
I will show how binary neutron star mergers...
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Myung-Ki Cheoun (Soongsil University)30/04/2026, 11:00
We investigate how density-dependent axial-vector coupling quenching and nucleon effective mass modify neutrino transport in core-collapse supernovae (CCSNe). We implement these in-medium effects in neutrino absorption, emission, and scattering opacities used by NULIB and perform simulations of the Woosley–Weaver 15M⊙ progenitor (s15s7b2) with the GR1D code. The effective-mass correction...
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Chang Ho Hyun (Daegu University)30/04/2026, 11:35
In this talk, we present recent developments of a new nuclear-matter equation of state (EoS) at finite density and temperature based on realistic nuclear interactions and density functional theory. It is argued that the nucleon effective mass plays an important role in determining the thermal stiffness of the EoS. The uncertainty associated with the in-medium effective mass is systematically...
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Chen Zhang (Tongji University)30/04/2026, 13:10
Some recent pulsar observations cannot naturally fit into the conventional picture of neutron stars: the compact objects associated with HESS J1731-347 and XTE J1814-338 have too small radii in the low-mass regime, while the secondary component of GW190814 is too massive for neutron stars to be compatible with constraints from the GW170817 event. In this study, we demonstrate that all these...
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Myungkuk Kim (CENS/IBS)30/04/2026, 13:45
Nuclear transport simulations are essential theoretical tools for exploring the properties of high-density nuclear matter. Numerous heavy-ion collision facilities around the world, such as RAON, RIKEN Nishina Center, and FRIB, are conducting a wide range of experiments, leading to the accumulation of extensive experimental data. In this context, the importance of nuclear transport...
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Hiroyuki Sako (JAEA)30/04/2026, 14:50
J-PARC is one of the world’s highest-intensity proton accelerators for material and life sciences, neutrino physics, and hadron and nuclear physics in a few ten GeV. J-PARC-HI (J-PARC Heavy-Ion Project) aims to accelerate heavy-ion beams at J-PARC, where we will introduce a heavy-ion injector consisting of a heavy-ion linac and a booster ring, while the heavy-ion beams are accelerated in the...
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Satomi Nakasuga30/04/2026, 15:25
The J-PARC E16 experiment aims to experimentally observe modifications of vector meson mass spectra in a nuclear medium, which are expected as a consequence of the partial restoration of chiral symmetry at finite density. In the experiment, vector mesons are produced by the 30 GeV proton beam at J-PARC on nuclear targets, and their di-electron decay is detected to obtain the invariant mass...
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Hidefumi Matsuda (Zhejiang University)30/04/2026, 16:00
We investigate the spectral function of the $\phi$ meson in hot and dense nuclear matter created in low-energy heavy-ion collisions, where the existence of the medium's rest frame leads to a splitting between the transverse and longitudinal modes of vector mesons. We compute the transverse and longitudinal spectral functions within the framework of QCD sum rules and apply them to the...
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Hirokazu Tamura (Tohoku University)01/05/2026, 09:00
Fifteen years have passed since the “hyperon puzzle” in neutron stars was raised, but it remains unsolved yet. Various experimental efforts have been and will be made to investigate hyperon-nucleon interactions in dense nuclear matter. Ξ hypernuclei as well as Λ hypernuclei have been intensively studied at J-PARC, clarifying an attractive Ξ-N interaction. High-quality Σ-N scattering...
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Asanosuke Jinno (Kyoto University)01/05/2026, 09:35
The appearance of hyperons in dense neutron-star matter strongly affects the corresponding equation of state. The onset density of hyperons depends on their single-particle potentials. In this talk, I report the single-particle potentials [1] of the $\Lambda$ and $\Sigma$ hyperons, calculated using up-to-date baryon–baryon interactions derived within chiral effective field theory up to...
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Yusuke Tanimura (Soongsil University)01/05/2026, 10:10
Terrestrial double-$\Lambda$ hypernuclear data and astronomical observations of neutron stars provide complementary constraints on the $\Lambda\Lambda$ interaction. In this work, we investigate the $\Lambda\Lambda$ interaction within a Skyrme energy density functional framework. We employ a Skyrme-type $\Lambda\Lambda$ interaction that includes the standard $s$- and $p$-wave terms, as well as...
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Kotaro Murakami (Institute of Science Tokyo)01/05/2026, 11:00
Interactions between a kaon and nucleon provide an essential input for understanding the partial restoration of chiral symmetry and the properties of pentaquarks. Although kaon-nucleon scattering experiments at low momenta have been performed since the 1960s, our understanding of these interactions remains limited due to the scarcity of experimental data near the threshold, which hampers a...
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Atsushi Hosaka (RCNP, Osaka University)01/05/2026, 11:35
We discuss hadron structure at low energies based on effective models. Conventional approach such as the quark model needs some updates in view of recent discoveries of non-conventional hadrons especially in resonance regions. The relevance of the chiral structure of resonances and impact on dense matter will be discussed.
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Philipp Gubler (JAEA)01/05/2026, 12:10
At present, there is no clear consensus regarding how the mass and width of
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the phi meson are modified in a dense environment such as nuclear matter,
nor on the strength of its chiral mixing with the axial-vector chiral
partner. Although a number of theoretical studies have addressed these
questions, establishing a direct connection with experimental observables
remains a significant... -
Toru Kojo (KEK)01/05/2026, 13:30
Recent observations of neutron stars, combined with causality, thermodynamic stability, and nuclear constraints, indicate a rapid stiffening of QCD matter at densities slightly above nuclear saturation density (n0 = 0.16fm-3). The evolution of the stiffening is faster than expected from purely nucleonic models with many-body repulsion. Taking into account the quark substructure of baryons, we...
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Hiroyuki Tajima (The University of Tokyo)01/05/2026, 14:05
The hadron-quark crossover (HQC) is one of the most exciting topics in nuclear astrophysics. Recently, microscopic features of HQC have been discussed in terms of the quarkyonic matter picture. In this talk, we address this problem from an Interdisciplinary context, by drawing an analogy with pairing fluctuations in the Bardeen-Cooper-Schrieffer to the Bose-Einstein condensate crossover,...
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Tsuyoshi Miyatsu (Soongsil University)01/05/2026, 14:40
We investigate dense nuclear matter within a unified framework that combines the quarkyonic picture with the quark-meson coupling (QMC) model, focusing on symmetric and isospin-asymmetric nuclear matter. Nucleons are described explicitly at the quark level using relativistic Gaussian quark wavefunctions, providing a microscopic realization of a dual baryon-quark description of dense matter....
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Nobutoshi Yasutake (Chiba Institute of Technology)01/05/2026, 15:00
We investigate the equation of state of neutron-star matter using color–spin molecular dynamics, explicitly incorporating the internal color and spin degrees of freedom of quarks and their dynamical evolution. Flavor conversion processes, including the emergence of strangeness, as well as beta equilibrium, are determined self-consistently through energy minimization. Our results show that, in...
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Prashant Thakur (Yonsei University)01/05/2026, 15:50
Abstract: Neutron stars provide a high-density laboratory to test dark matter (DM) through its gravitational imprint on stellar structure and early evolution. In this talk, I present a unified set of results based on two-fluid modeling of cold neutron stars and evolving proto-neutron stars (PNSs), together with Bayesian model selection, multi-messenger constraints, and inverse parameter...
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Yeunhwan Lim (Yonsei University)01/05/2026, 16:25
We study how the nuclear symmetry energy and its density slope parameter affect the neutron dripline of finite nuclei and the macroscopic properties of neutron stars within a semiclassical liquid drop model (LDM). Our analysis employs energy density functionals constrained by chiral effective field theory. The symmetry energy at saturation density is fixed, while the surface tension parameter...
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LIU Xiang01/05/2026, 17:00
This work focuses on the existence of pion condensate in neutron star matter based on a parity doublet model. Parity doublet model is a model that explains the hadron mass as two parts: one part is generated by spontaneous breaking of chiral symmetry and the other is an invariant mass that does not depend on the breaking of chiral symmetry and is called a chiral invariant mass $m_0$. A pion...
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Vivek Baruah Thapa (Birangana Sati Sadhani Rajyik Vishwavidyalaya)01/05/2026, 17:20
We present a unified Bayesian analysis of the dense-matter equation of state (EOS) of neutron stars by incorporating exotic hadronic degrees of freedom, namely antikaon condensation and Δ-resonances, within a density-dependent relativistic hadron framework. The model is constrained using nuclear saturation properties, chiral effective field theory ($\chi$EFT) calculations for symmetric and...
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Hao-Song You (Tsung-Dao Lee Institute, Shanghai Jiao Tong University)01/05/2026, 17:40
Using an equivparticle model with mean-field approximation (MFA), we systematically investigate quark matter properties across scales, from microscopic multibaryon states to macroscopic compact dwarfs. First, we determine the mass spectra of color-singlet $N$-quark configurations ($N=3$ to $18$) based on SU(6) symmetry and Bayesian inference. Our results predict several bound states, including...
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Kazuyuki Sekizawa (Institute of Science Tokyo)02/05/2026, 09:00
Neutron stars can be regarded as natural laboratories to explore physics of many-nucleon systems from sub- to supra-saturation densities. We aim to understand various macroscopic astrophysical phenomena of neutron stars based on microscopic theories. In this talk, I will review recent activities in our nuclear theory group at Science Tokyo (see, e.g., Refs. [1-8]) and discuss selected topics...
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Valentin Allard (Yonsei University)02/05/2026, 09:35
Born from gravitational-core collapse supernovae, with initial temperatures as high as $\sim10^{12}$K, neutron stars cool down to temperatures $10^9$K within a few days, providing a unique opportunity to explore matter under extreme conditions. In particular, neutron stars contain nuclear superfluids whose presence is supported by observations of pulsar frequency glitches, rapid decline in...
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Tomoyuki Maruyama (College of Bioresource Sciences, Nihon University)02/05/2026, 10:10
The origin of ultra–high–energy cosmic rays (UHECRs), including the $2.44\times10^{20}$ eV event detected by AMATERAS, remains an open problem in astrophysics. Strong magnetic fields, such as those associated with magnetars, are expected to play an important role both in accelerating particles to ultra–high energies and in shaping the accompanying radiation. In such environments, synchrotron...
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Sachiko Tsuruta (Montana State Univrsity)02/05/2026, 11:00
We will review recent developments in the problems of thermal evolution of neutron stars and other related objects. Since the first discovery of a neutron star, over years we have seen significant developments in the understanding of these stars, through advancement in both theory and observation. Consequently, we now have better hope for the understanding of high density matter beyond the...
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Hao Sun (扬州大学)02/05/2026, 11:35
Employing relativistic energy density functionals PKDD, DD-ME2, and TW99 for nucleon-nucleon interactions, we investigate the impact of $\Delta$ resonances on the frequencies of non-radial $g$-mode oscillations in neutron stars adopting the universal coupling scheme. Our results show that when the proportion of $\Delta$ resonances in the neutron star interior reaches a certain threshold, the...
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Akira Dohi (RIKEN)02/05/2026, 11:55
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
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isolated neutron stars beyond the standard cooling scenario without rapid cooling (i.e., minimal cooling... -
Toshitaka Tatsumi (home)02/05/2026, 13:15
Origin of the strong magnetic field observed in compact stars has been an interesting issue. If nuclear matter favors spin polarization, it gives a possible origin of the magnetic field. However, any realistic calculation has not given positive results. We discuss some microscopic origin of the magnetic field in dense quark matter. We consider here two types of chiral transitions, dual chiral...
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JiaXing Niu (Yangzhou university)02/05/2026, 13:50
Data tables on the equation of state (EOS) and microscopic structures for dense stellar matter under both cold and finite-temperature conditions with proton fractions $Y_p =0.01$-$0.65$ and baryon number densities $n_\text{b}=10^{-8}$-$2 \ \mathrm{fm}^{-3}$ are obtained adopting two classes of relativistic density functionals, namely, those with nonlinear self-couplings and those with...
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Cheng-Jun Xia (Yangzhou University)02/05/2026, 14:10
The properties of magnetized dense stellar matter in white dwarfs and neutron star crusts are investigated in a fully three-dimensional geometry with periodic boundary condition. The Thomas-Fermi approximation is employed to fixed the electron density profiles, while the nonuniform magnetic fields are treated with equivalent magnetic charge method.
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02/05/2026, 15:10
Toshiki Maruyama
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Young-Ho Song (IRIS, IBS)
We performed ab initio nuclear lattice calculations of the neutron-rich carbon and oxygen isotopes using high-fidelity chiral interactions and found good agreement in binding energy. We discuss correlations associated with each two-nucleon interaction channel.
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Helei Liu
Thermonuclear (Type I ) X-ray bursts from accreting neutron stars offer a means to determine neutron-star (NS) mass ($M$) and radius ($R$) and thereby probe the properties of matter at supranuclear density. A subset of these events, photospheric radius–expansion (PRE) bursts, provide a particularly powerful tool to constrain the neutron-star $M$ and $R$. Here, we apply the direct cooling-tail...
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Keita Izumi (Kobe University)
Several indirect observations imply that the central compact object in the supernova SN 1987A is likely to be the youngest neutron star NS 1987A. Although no direct observation on the NS 1987A has been made yet, a future high-resolution X-ray satellite, such as the Lynx, could potentially detect its thermal emission. We investigate when the NS 1987A can be detected with the use of Lynx,...
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