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David Rapagnani (University of Naples "Federico II")10/21/26, 6:00โฏPMUnderground nuclear astrophysicsPoster Presentation
$\rm^{24}Mg(p,\gamma)^{25}Al$ plays a key role in the MgโAl cycle, e.g. influencing the chemical evolution of asymptotic giant branch stars and the nucleo-synthesis of intermediate-mass nuclei, notably $\rm ^{26}$Al.
Despite its relevance, the reaction rate at stellar energies remains poorly constrained due to the extremely low cross sections within the sub-resonant Gamow window.In this...
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Sayan Samanta (Bose Institute, Kolkata, India)10/21/26, 6:00โฏPMPoster Presentation
The cosmological lithium problem [1] remains one of the major unresolved issues in nuclear astrophysics. It is related to the production and destruction channels of primordial $^{7}$Be, the main source of $^{7}$Li. Though the production channels of $^{7}$Be are well studied [2], improved measurements are required in the destruction reactions. The dominant neutron-induced destruction channels,...
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Myung-Ki CHEOUN (Soongsil University)10/21/26, 6:00โฏPMPoster Presentation
We present neutrino-transport calculations for core-collapse supernova explosions (CCSNe), treating both degenerate and non-degenerate baryonic matter. Because neutrinoโnucleon interactions are strongly affected by baryon degeneracy through Pauli blocking, the high-density region near the neutrinosphere requires careful phase-space integrations for the participating nucleons.
To address...
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Dayoung Byun (Chungnam National University)10/21/26, 6:00โฏPMPoster Presentation
We present a chemo-kinematic study of an extremely metal-poor giant LAMOST J015857.38+382834.7 (hereafter J0158) with [Fe/H] = -3.46. J0158 shows an unusual light-element pattern, with strong Na enhancement but no strong carbon enhancement, consistent with globular cluster-like second-population chemistry. Its high [Eu/Fe] = +1.6, and low Ba abundance classify it as a strongly...
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Mr Jaehyun Kim (Chungnam National University)10/21/26, 6:00โฏPMPoster Presentation
NGC 1978 is one of the youngest massive globular clusters (GCs) in the Large Magellanic Cloud, with reported photometric multiple-population (MP) signatures. We present a high-resolution near-infrared abundance analysis of 19 red giant branch-like stars in NGC 1978 using H- and K-band IGRINS spectra. Stellar parameters and abundances of C, N, O, Na, Mg, Al, Si, Ca, Ti, and Ce were derived...
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Xinxu Wang (Beihang University), Yudong Luo10/21/26, 6:00โฏPMPoster Presentation
The $^{176}$Lu ($t_{1/2}\sim$36 Gyr) and $^{176}$Hf are only produced by the main component of the slow neutron capture process (main $s$-process) in AGB stars.
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The nucleosynthesis of the isomeric state of $^{176}$Lu$^{m}$ ($t_{1/2}\sim$3 h) dominates the $^{176}$Lu/$^{176}$Hf ratio because it cannot reach the thermal equilibrium with the ground state $^{176}$Lu$^{g}$ at the temperature of... -
Miji Jeong (Korea Astronomy and Space science Institute (KASI))10/21/26, 6:00โฏPMPoster Presentation
We present a detailed chemical abundance analysis of LAMOST J122216.86โ063345.26 (J1222), an actinide-boost r-I star observed with Gemini-S/GHOST. J1222 is a very metal-poor giant with [Fe/H] = โ2.45 and is dynamically associated with the Iโitoi substructure, making it a valuable tracer of early chemical enrichment in a system accreted into the Milky Way. From 43 measured elements, we find...
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Amira Aoyama (Tokyo University of Science / RIKEN)10/21/26, 6:00โฏPMPoster Presentation
X-ray bursts are thermonuclear explosions that occur when accreted material on the surface of a neutron star reaches critical conditions. Superbursts are exceptionally energetic events, lasting several hours or longer and releasing more than two orders of magnitude more energy than ordinary X-ray bursts. They are thought to involve carbon burning. Previous studies have suggested that the fuel...
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Tomoshi Takeda (Kyoto University)10/21/26, 6:00โฏPMPoster Presentation
Type-I X-ray bursts are thermonuclear explosions on the surfaces of accreting neutron stars (NSs). During these bursts, the rapid proton-capture process (rp-process) is thought to synthesize heavier nuclei and leave observable imprints on the burst light curves. While most X-ray bursters exhibit irregular burst recurrence times and profiles, only a few sources, known as โclockedโ bursters,...
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Giuseppe Gabriele Rapisarda (DFA-UniCT & LNS-INFN)10/21/26, 6:00โฏPMPoster Presentation
ฮณ-induced reactions like (ฮณ, n), (ฮณ, p), and (ฮณ, ฮฑ) are of interest in several astrophysical scenarios such as Big Bang Nucleosynthesis and the Li-problem, Si-burning in massive stars, p-process. Recently, the ASFIN collaboration, in the framework of an international collaboration, has started an experimental campaign at the High Intensity Gamma-Ray Source (HIฮณS) dedicated to the study of...
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Jun-yao Xu (Beihang University)10/21/26, 6:00โฏPMPoster Presentation
We found that a heavy target such as Pb is most suitable for determining the proton distribution radii of unstable nuclei through charge-changing cross-section ($\sigma_\text{cc}$) measurements. As a heavy ion probe, low-$Z$ targets are routinely used to determine nucleon distribution radii of unstable isotopes. This approach has recently been extended to study proton distribution radii from...
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Hongrui Feng (Beihang University), Yudong Luo10/21/26, 6:00โฏPMPoster Presentation
The discrepancy between the observationally inferred primordial 7Li abundance and the theoretical prediction of Standard Big Bang Nucleosynthesis (SBBN) remains one of the longstanding unsolved problems in modern cosmology. In addition, recent spectroscopic observations of metal-poor extra-galactic systems have reported a lower primordial 4He abundance than previously reported from...
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Young Sun Lee (Chungnam National University)10/21/26, 6:00โฏPMPoster Presentation
We present a chemical and dynamical analysis of 22 metal-poor stars with [Fe/H] < โ1.0 selected from Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST). High-resolution spectra were obtained with Gemini-N/GRACES and Gemini-S/GHOST, enabling the determination of stellar atmospheric parameters and elemental abundances spanning light, ฮฑ, iron-peak, and neutron-capture elements....
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Tong Zhang (Institute of Modern Physics, Chinese Academy of Sciences)10/21/26, 6:00โฏPMPoster Presentation
ฮฝp-process in supernovae produces light p-nuclei. The (n,p) reactions on Ge isotopes control how much matter flows toward heavy nuclei, but existing reaction rates rely on phenomenological models with unknown uncertainties.
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We computed new (n,p) reaction rates in the Ge-Ga region using microscopic optical potentials derived from chiral nuclear forces, compared them with the standard JINA... -
Kosei Nagao (Kyoto University)10/21/26, 6:00โฏPMPoster Presentation
The $^{12}\mathrm{C} + ^{12}\mathrm{C}$ fusion reaction plays a key role in several astrophysical explosive phenomena. However, the cross section for the $^{12}\mathrm{C} + ^{12}\mathrm{C}$ fusion reaction at the relevant energy region is difficult to determine because of both experimental limitations and strong resonant structures. We develop a reaction model that explicitly treats the...
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Kanji Mori (Fukuoka University)10/21/26, 6:00โฏPMPoster Presentation
Core-collapse supernovae are powerful cosmic laboratories to probe physics beyond the Standard Model. While exotic particles can alter explosion dynamics, previous studies relying on post-processing could not fully capture the non-linear feedback on multi-dimensional hydrodynamic features. In this talk, we report constraints on new physics obtained through two-dimensional neutrino-radiation...
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Dr Kazuyuki Sekizawa (Institute of Science Tokyo)10/21/26, 6:00โฏPMPoster Presentation
The rapid cooling observed in the Cassiopeia A neutron star (CasA NS) is one of the most stringent tests for neutron-star cooling theory. While Cooper-pair breaking and formation (PBF) neutrino emission is a leading candidate, uncertainties remain regarding the PBF efficiency factor $q$ and the neutron ${}^3$P${}_2$ pairing gap. This work [1] explores in a data-driven manner how the optimized...
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Dr Soomi Cha (Center for Exotic Nuclear Studies, Institute for Basic Science)10/21/26, 6:00โฏPMPoster Presentation
Investigating (ฮฑ,p) reactions is essential for understanding explosive stellar environments, such as X-ray bursts and core-collapse supernovae. However, direct measurements of (ฮฑ,p) reactions with rare-isotope beams remain experimentally challenging, and previous studies have therefore relied largely on theoretical estimates and indirect approaches. An Active Target Time Projection Chamber...
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Grant Mathews (University of Notre Dame)10/21/26, 6:00โฏPMPoster Presentation
A first order phase transition to quark matter can provide a shock revival mechanism for core-collapse supernovae and a means to enhance the energy of the explosion. Recent studies have also noted the onset of radial oscillations of the core that can be excited when the equation of state allows the formation quark matter. Such oscillations may produce an observable signal in emitted neutrinos....
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Tejpreet Kaur (Indian Institute of Technology Kanpur, India)10/21/26, 6:00โฏPMPoster Presentation
Nucleosynthetic yields from stars are key inputs for galactic chemical evolution models and are essential for understanding the origin and distribution of elements in galaxies. While most chemical evolution studies adopt single-star yields for massive stars, observations indicate that the majority of massive stars form and evolve in binary systems. Incorporating the effects of binary evolution...
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Taeho Lee (Institute of Science Tokyo)10/21/26, 6:00โฏPMPoster Presentation
The observations of massive neutron stars provide a stringent constraint on the nuclear matter equation of state (EoS). While exotic particles such as hyperons may emerge in high-density neutron-star matter, their appearance generally softens the EoS, making it difficult to sustain neutron stars with masses of $2M_\odot$ or heavier. This apparent inconsistency between hyperonic EoS models and...
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Prof. Takumi Muto (Chiba Institute of Technology)10/21/26, 6:00โฏPMPoster Presentation
Thermal evolution of neutron stars, as well as mass and radius observations, brings about important astrophysical information on properties of highly dense matter in inner core of a neutron star. As a candidate of novel hadronic phase, a coexistent phase of kaon condensation and hyperon-mixed matter [abbreviated to (Y+K) phase] has been extensively studied from both theoretical and...
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Tatsuya Matsuki (The University of Tokyo)10/21/26, 6:00โฏPMPoster Presentation
We investigate the possible impact of multineutron states on nuclear composition under conditions relevant to core-collapse supernovae and proto-neutron stars. We examine the role of multineutron states, such as dineutrons and tetraneutrons, which may emerge from neutron correlations in neutron-rich matter.ย We extend a statistical model of nuclear matter by incorporating dineutron and...
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Tsuneo NODA (Kurume Institute of Technology)10/21/26, 6:00โฏPMPoster Presentation
Compact objects such as neutron stars are composed of matter so dense that they can be likened to a single, massive atomic nucleus. The density at their cores exceeds that of a nuclear nucleus, and it is predicted that various states of matterโnot found in ordinary atomic nucleiโwill emerge there. The state of matter within these objects has a significant impact on neutrino emission, which can...
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Prof. Hajime SOTANI (Kochi University)10/21/26, 6:00โฏPMPoster Presentation
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 $K_0$, we constrain the mass and radius of an extragalactic neutron star at redshift $z=0.13$. Identifying the low-order...
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Thomas Chillery (University of Naples)10/21/26, 6:00โฏPMPoster Presentation
Around half the elements heavier than iron originate from the astrophysical slow neutron-capture (s-) process. This mechanism occurs within the stellar environments of asymptotic giant branch and massive stars, where the endothermic 22Ne(ฮฑ,n)25Mg reaction is one of the main sources of neutrons. This reaction competes with 22Ne(ฮฑ,ฮณ)26Mg across the astrophysical temperature regime 150 โ 300 MK...
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Ryota Hatami (SOKENDAI/NAOJ)10/21/26, 6:00โฏPMPoster Presentation
A massive star explodes as a core-collapse supernovae at the end of life and the explosion can be observed as a supernova remnant (SNR) over up to about ten thousand years. The elemental abundances observed in SNRs provide important clues to both nucleosynthesis in pre-supernova evolution and the supernova explosion. Recent observations of Cassiopeia A (Cas A), which is one of the best-studied...
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Liu Jiabao (Waseda University)10/21/26, 6:00โฏPMPoster Presentation
Core-collapse supernovae are promising sites of explosive nucleosynthesis, where the electron fraction of the ejecta is strongly influenced by the spectra and angular distributions of electron neutrinos and antineutrinos. Recent multidimensional simulations suggest that fast neutrino flavor conversion can occur in the decoupling region of core-collapse supernovae, potentially modifying the...
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Grant Mathews (University of Notre Dame)10/21/26, 6:00โฏPMPoster Presentation
We analyze the chemical evolution of alpha elements and iron for sumulated dwarf galaxies in Milky-Way-like plane-of-satellite systems for the TNG50 large-scale cosmological simulation. We first analyze the formation of the 11 most lumious satelites that form the plane of satellites around the MIlky Way. Having identified simulated systems that match the properties of the Milky-Way...
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Benjamin Wehmeyer (University of Wrocลaw)10/21/26, 6:00โฏPMPoster Presentation
The origin of the heaviest elements is still a matter of debate. For the rapid neutron capture process (r-process), multiple sites have been proposed, e.g., neutron star mergers and (sub-classes) of supernovae. R -process elements have been measured in a large fraction of metal-poor stars. Galactic archaeology studies show that the r-process abundances among these stars vary by over 2 orders...
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Benjamin Wehmeyer (University of Wrocลaw)10/21/26, 6:00โฏPMPoster Presentation
Studying the galactic chemical evolution with short lived radioisotopes (SLRs) has a significant advantage over using stable elements: Due to their radioactive decay, SLRs carry additional timing information on astrophysical nucleosynthesis sites.
We can use meteoritic abundance data in conjunction with a chemical evolution model to constrain the physical conditions in the last rapid...
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Chang Mok Do (Chungnam National University)10/21/26, 6:00โฏPMPoster Presentation
Metal-poor stars preserve fossil records of early nucleosynthesis and the chemical evolution of the Milky Way (MW). Carbon-enhanced metal-poor (CEMP) stars are especially useful tracers of the MWโs earliest enrichment. We obtained medium-resolution (R ~ 4000) spectra with Gemini/GMOS for a sample of bright CEMP candidates selected from the LAMOST survey. We derive stellar atmospheric...
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Ryo Ishikawa (Tohoku University)10/21/26, 6:00โฏPMPoster Presentation
The earliest chemical enrichment in the Universe was driven by supernovae of Population III stars. Low-mass second-generation stars formed from gas polluted by these ejecta can survive to the present day as extremely metal-poor (EMP) stars in the Galactic halo. Their abundance patterns provide a fossil record of early nucleosynthesis and chemical evolution. However, an observed EMP star may...
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MIN ZHANG (Institute of Modern Physics, Chinese Academy of Sciences)10/21/26, 6:00โฏPMPoster Presentation
The recent mass measurement of $^{70}$Kr using the $B\rho$-defined isochronous mass spectrometry yields a mass excess of $-41320(140)$ keV, indicating a 220-keV increase in binding energy compared to the AME2020 prediction. We utilize this experimental mass to probe its impact on the potential waiting point $^{68}$Se in $r$p-process and quantitatively constrain the $2p$-capture reaction...
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AZNI ABDUL AZIZ (INTERNATIONAL ISLAMIC UNIVERSITY MALAYSIA)10/21/26, 6:00โฏPMPoster Presentation
The 12C+12C fusion reaction plays a crucial role in stellar carbon burning and the evolution of massive stars. However, significant uncertainties remain in the fusion cross sections and reaction rates at astrophysical energies. In this work, we systematically investigate the performance of various versions of the proximity potential formalism in describing the 12C+12C fusion process. Fusion...
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Dr Nobuya Nishimura (Kogakuin University)10/21/26, 6:00โฏPMPoster Presentation
Nucleosynthesis in Type I X-ray bursts, particularly the rp-process, provides an important connection between nuclear physics and astrophysical observations. However, many reaction rates relevant to explosive hydrogen burning remain experimentally unconstrained, and theoretical predictions still involve substantial uncertainties. We investigate the astrophysical impact of a newly calculated...
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Tatsuhiro Hattori (Institute of Science Tokyo)10/21/26, 6:00โฏPMPoster Presentation
Pulsar glitches are sudden quasi-periodic increases in the rotation frequency of neutron stars, and are believed to originate from the dynamics of quantized vortices in the neutron superfluid interior. Recently, the vortex network model proposed by Marmorini et al.(2024) suggested that the coupling between $^3P_2$ half-quantized vortices (HQVs) in the outer core and $^1S_0$ singly-quantized...
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Yuki Yamanouchi (Kyushu University)10/21/26, 6:00โฏPMPoster Presentation
The rapid neutron-capture process (r-process) is considered responsible for the production of approximately half of the elements heavier than iron in the universe. However, theoretical predictions of r-process abundance patterns still suffer from large uncertainties because experimental nuclear data for neutron-rich nuclei, including atomic masses, $\beta$-decay half-lives, and...
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Mr Yu An (TU Darmstadt, HFHF)10/21/26, 6:00โฏPMPoster Presentation
Neutron capture rates play an important role in shaping r-process patterns and are commonly calculated within the Hauser-Feshbach statistical model. Their predictions depend on nuclear masses, nuclear level densities, ฮณ-ray strength functions, and optical potentials. We investigate how uncertainties in these statistical model inputs propagate to r-process nucleosynthesis by calculating neutron...
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Koya Chiba (Tohoku University)10/21/26, 6:00โฏPMPoster Presentation
Radioactive decay in material ejected from a binary neutron star (BNS) merger powers a thermal transient known as a kilonova. Following the detection of the gravitational-wave event GW170817, the associated kilonova AT2017gfo was observed. This event provided the first opportunity for spectroscopic studies of freshly synthesized $r$-process material. Although several absorption and emission...
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Dr Shin-ichiro Fujimoto (Kumamoto national college of technology)10/21/26, 6:00โฏPMPoster Presentation
A magnetar is a neutron star whose surface magnetic field is typically stronger than $10^{13}\,{\rm G}$. Its large magnetic energy powers outbursts in the X-ray to $\gamma$-ray bands. The most energetic class of such bursts, with released energies of $10^{44}$--$10^{47}\,{\rm erg}$, is called a giant flare (GF). Radio afterglows detected from two Galactic GFs suggest the presence of massive,...
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Yudong Luo10/21/26, 6:00โฏPMPoster Presentation
Type I X-ray bursts provide an important site for rp-process nucleosynthesis, where reaction flows are strongly influenced by nuclear masses, beta-decay lifetimes, and possible isomeric states. In this talk, I will present recent studies on the impact of new precision mass measurements, including 70Kr near the 68Se waiting point and nuclei in the A๏ฝ90โ100 region, on X-ray burst light curves...
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Mr Pranav Nalamwar (University of Notre Dame)10/21/26, 6:00โฏPMPoster Presentation
Simulating nucleosynthesis requires an accurate evolution of temperature and density within astrophysical environments. Contemporary nuclear networks typically post-process tracers from astrophysical simulations and assume the energy generated by nuclear heating is the dominant source of entropy change along the tracer. However, such a procedure neglects entropy changes embedded in the tracer...
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Kai Matsunaga (Kyoto University)10/21/26, 6:00โฏPMPoster Presentation
Chlorine (Cl) and potassium (K) are essential elements for life, yet their cosmic origins remain poorly understood. Current Galactic chemical evolution models underestimate the production of Cl and K by up to an order of magnitude (e.g., Kobayashi et al. 2020). However, these light odd-Z elements have not been clearly detected at their production sites, preventing direct observational tests of...
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Shota Wajima (Kyoto University)10/21/26, 6:00โฏPMPoster Presentation
Metal-poor stars preserve chemical abundance patterns imprinted by nucleosynthesis in the early Universe, providing key constraints on the evolution and explosions of massive stars at extremely low metallicity. Among these abundance ratios, [Na/Mg] exhibits a particularly large scatter (Ishigaki et al. 2026). Sodium is mainly produced during carbon burning, and its yield can be predicted more...
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Xuan Pang (Beihang University)10/21/26, 6:00โฏPMPoster Presentation
We report the new measurement of the photoneutron reaction for $^{45}$Sc performed using the quasi-monoenergetic $\gamma$-ray beam at the Shanghai Laser Electron Gamma Source (SLEGS). The obtained cross sections achieve an overall uncertainty better than 4\%. Compared with previous experimental data, the present results are systematically higher by a factor of approximately 1-2. By combining...
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Dr Jung Woo Lee (Center for Exotic Nuclear Studies, Institutes for Basic Science)10/21/26, 6:00โฏPMPoster Presentation
Proton-induced inelastic scattering to the $^{12}$C Hoyle state (7.654 MeV), which de-excites $^{12}$C to its ground state by carrying away the excitation energy โ a process known as "upscattering" โ may enhance the stellar triple-alpha process by up to orders of magnitude. The triple-alpha enhancement was predicted using previous measurements of the time-reversed reaction...
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Tatsushi Shima (Research Center for Nuclear Physics, Osaka University)10/21/26, 6:00โฏPMPoster Presentation
In core-collapse supernova explosions, the energy transfer from neutrinos to matter (neutrino heating) is considered a key ingredient of the explosion mechanism. However, even after taking into account multidimensional hydrodynamics, magnetic fields, turbulence, and realistic nuclear equations of state, reproducing robust explosions over a wide range of progenitors remains challenging.
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Janka... -
Tomoyuki Maruyama (College of Bioresource Sciences, Nihon University)10/21/26, 6:00โฏPMPoster Presentation
The origin of ultra-high-energy cosmic rays (UHECRs), such as the recent $2.44ร10^{20}$ eV "Amaterasu" event detected by the Telescope Array, remains one of the most intriguing mysteries in astrophysics. Identifying the sources of these particles is challenging because their trajectories are significantly deflected by cosmic magnetic fields. A promising approach to identifying UHECR sources is...
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Bakuh Danang Setyo Budi (SOKENDAI/NAOJ)10/21/26, 6:00โฏPMPoster Presentation
Oxygen abundances in very and extremely metal-poor (V/EMP) stars provide critical constraints on early massive stars' nucleosynthesis. We present an oxygen abundance analysis for 35 V/EMP stars ($-4.0<\text{[Fe/H]}<-1.5$) using near-infrared $H$-band OH lines from high-resolution Subaru/IRD spectra. To evaluate these atmospheric diagnostics, we compare OH-based abundances against the...
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Tsurugi Takata (Fukuoka University)10/21/26, 6:00โฏPMPoster Presentation
Supernovae realize extreme environments of high temperature and high density, serving as useful astrophysical laboratories for probing feebly interacting new particles such as axion-like particles (ALPs). In this work (arXiv:2604.17840 [astro-ph.HE]), we investigate how rotation modifies the constraints on MeV-scale ALPs coupled to photons derived from SN 1987A. We constrain the ALP parameter...
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Zhenyu He (China Institutu of Atomic Energy)10/21/26, 6:00โฏPMPoster Presentation
The origin of heavy elements via the r-process remains a frontier in nuclear astrophysics. While neutron star mergers (NSMs) are confirmed sites, collapsars and magnetohydrodynamically driven jets (MHDJs) offer unique environments due to their distinct jet dynamics.
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We discover for the first time that fission neutrons released after the r-process freeze-out can induce secondary i- and... -
Prof. Kawchar Patwary (Comilla University)10/21/26, 6:00โฏPMPoster Presentation
Neutron-capture cross sections are essential nuclear physics inputs for modeling the s-process nucleosynthesis, which is responsible for producing approximately half of the elements heavier than iron in the Universe. The isotope
Go to contribution page{}^{191}_{77}\mathrm{Ir}plays an important role in the s-process because neutron capture on$^{191}\mathrm{Ir}$produces$^{192}\mathrm{Ir}$, a branching-point... -
Prof. Rosario Gianluca Pizzone (Universitร di Catania & INFN-LNS)10/21/26, 6:00โฏPMPoster Presentation
The neutron-capture reaction $^{84}$Kr(n,$\gamma$)$^{85}$Kr plays an important role in the astrophysical s-process, where $^{85}$Kr acts as a key branching-point nucleus influencing the production of isotopes in the mass region around Sr and Rb. Since direct measurements of this reaction are experimentally difficult, an indirect approach based on the Asymptotic Normalization Coefficient (ANC)...
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Gyoungmo Gu (Sungkyunkwan University,Center for Exotic Nuclear Studies, Institute for Basic Science)10/21/26, 6:00โฏPMPoster Presentation
Particle-hole excitations near closed nuclear shells provide important information on single-particle properties, shell evolution, and residual two-body interactions. While doubly magic and near-doubly magic nuclei have been extensively studied, charge-changing particle-hole excitation states in $^{48}$Ca, corresponding to negative-parity T=5 states, remain less well established. These states...
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Riccardo Maria Gesuรจ (Gran Sasso Science Institute (GSSI), INFN LNGS)10/21/26, 6:00โฏPMPoster Presentation
Carbon burning is a crucial stage of stellar evolution, determining whether stars evolve toward neutron stars, black holes, or CO white dwarfs. These outcomes depend strongly on the $^{12}C+^{12}C$ reaction rate, which is still uncertain at astrophysical energies.
This reaction mainly proceeds through the $^{12}C(^{12}C,\alpha)^{20}Ne$ and $^{12}C(^{12}C,p)^{23}Na$ channels. While it has...
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Dr Akira Dohi (RIKEN)10/21/26, 6:00โฏPMPoster Presentation
In accreting neutron stars, rapidly brightening phenomena have often been observed, so-called Type-I bursts. Most of them are observed in a hard state, that is, a relatively dark phase. In the hard state, most observations show an inverse relation between burst recurrence time and accretion rate, which is in line with conventional burst models.
Recently, many bursters have been observed...
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Dr Zifeng Luo (Institute for Basic Science)10/21/26, 6:00โฏPMPoster Presentation
We investigate the $^{13}\mathrm{C}(^{12}\mathrm{C},n)^{24}\mathrm{Mg}^*$ reaction as a neutron-spectator Trojan Horse Method (THM) route to low-energy $^{12}\mathrm{C}+{}^{12}\mathrm{C}$ fusion, using the physical $^{13}\mathrm{C}=^{12}\mathrm{C}+n$ $p_{1/2}$ overlap. For a 27 MeV $^{12}\mathrm{C}$ beam and $0.8\leq E_{CC}\leq2.7$ MeV, the momentum-volume density peaks at $72.5$ MeV/$c$, with...
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Kei Sato (The University of Osaka)10/21/26, 6:00โฏPMPoster Presentation
Primitive meteorites contain nanometer- to micrometer-sized grains that exhibit isotopic anomalies in various elements relative to the solar system composition. These grains, known as presolar grains, preserve isotopic signatures that reflect nucleosynthesis in the stellar sources before the formation of the solar system. High-precision trace element isotopic analyses of presolar grains...
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Azusa Inoue10/21/26, 6:00โฏPMPoster Presentation
The aim of our research is to achieve a comprehensive understanding of the Big Bang Nucleosynthesis (BBN) process and to potentially resolve the Cosmological Lithium Problem (CLP). The CLP is a well-known issue in astrophysics, referring to the overestimation of the primordial $^7\mathrm{Li}$ abundance in standard BBN models compared to astronomical observations. One of the major challenges in...
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Ainun-Nahdhia Azhari10/21/26, 6:00โฏPMPoster Presentation
While the r-process yield, especially the actinide-to-lanthanide abundance ratio, has been widely studied in metal-poor stars, their evolution in the metal-rich regime is poorly understood. One cause is the limited Th abundance measurement due to the difficulty of detecting the commonly used Th II 4019 ร absorption line in stellar spectra.
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In this study, we present the [Th/Eu] ratio... -
marco la cognata (infn-lns)10/21/26, 6:00โฏPMPoster Presentation
Our recent work [1] investigates the 16O+16O fusion reaction, a critical process for understanding how massive stars burn oxygen during their final evolutionary stages. Because direct measurements at low stellar energies are difficult to obtain, researchers performed a validity test using the Trojan Horse Method to study the reaction indirectly. The study specifically explores using 20Ne as a...
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Prantik Sarmah (Institute of High Energy Physics, Beijing)10/21/26, 6:00โฏPMPoster Presentation
The detection of near-TeV gamma rays from the 2021 outburst of RS Oph ($2.45$ kpc) by MAGIC established recurrent novae as Galactic TeV particle accelerators. However, the underlying emission mechanismโhadronic or leptonicโremains unresolved due to the absence of coincident neutrino detections. The anticipated outburst of the much closer recurrent nova T Coronae Borealis (T CrB, $\sim0.887$...
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Prof. Toshio Suzuki (Nihon University)10/21/26, 6:00โฏPMPoster Presentation
Nuclear Urca processes play important roles in the cooling of stars. Electron-capture and $\beta$- decay rates of the nuclear pairs, $^{25}$Mg-$^{25}$Na and $^{23}$Na-$^{23}$Ne, were evaluated by the shell model, and successfully applied to the cooling of O-Ne-Mg cores of stars with M$_{\odot}$ [1]. The Urca processes were shown to induce the cooling of neutron star (NS) crusts [2], where the...
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Peter Moller (Lund University)10/21/26, 6:00โฏPMPoster Presentation
To discuss the determination of model errors we use for simplicity mass models ("mass tables"). Usually their errors are characterized by the root-mean-square deviation $ \sigma_{\mathrm{rms}} = \left( \left[ \sum_{i = 1}^n \left( M_{\mathrm{exp}}^i - M_{\mathrm{th}}^i \right)^2 \right] / n \right)^{1/2} $. However, we immediately (should) see
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that the experimental error contributes to the...
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