Conveners
Session 1
- Hajime Sotani (Kochi University)
Session 1
- There are no conveners in this block
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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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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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