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Chris Fryer (Los Alamos National Laboratory)26/05/2026, 09:00Invited talk (30min + 10min Q&A)
A number of supernova engines are thought to contribute to the growing menagerie of transients produced by stellar collapse. Gamma-ray observations of the decay of radioactive isotopes provide one of the most direct probe of these engines with the potential to not only distinguish between different engines but also probe the nature of specific engines. Here I review the differences in the...
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Ryota Hatami (SOKENDAI/NAOJ)26/05/2026, 09:40Contributed talk (15min + 5min Q&A)
A core-collapse supernova (CCSN) is an explosion of a massive star at the end of their life. The explosion mechanism has not yet been clarified in spite of studies for long time. In this study, we focus on nucleosynthesis as a clue to understand the explosion mechanism. Because CCSNe have driven chemical evolution of the Universe, metal-poor stars born in the early Universe remain the...
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Zhenghai Liu (North Carolina State University)26/05/2026, 10:00Contributed talk (15min + 5min Q&A)
We consider the question of whether core-collapse supernovae (CCSNe) can produce rapid neutron
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capture process (r-process) elements and how future MeV gamma-ray observations could address this.
Rare types of CCSNe characterized by substantial magnetic fields and rotation, known as magnetorotational supernovae (MR-SNe), are theoretically predicted to produce these elements, although... -
Stephen J. Mojzsis (University of Bayreuth, Bavarian Geoinstitute (BGI))27/05/2026, 09:00Invited talk (30min + 10min Q&A)
The thermal evolution of rocky exoplanets is modulated by (i) left-over (gravitational) heat of accretion, and (ii) radiogenic heating from the decay of long-lived radioactive isotopes, particularly 40^K, 232^Th, 235^U, and 238^U. These heat-producing elements (HPEs) are synthesized through distinct nucleosynthetic pathways and evolved in both relative and absolute abundance over time as...
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Luca Boccioli (UC Berkeley)27/05/2026, 09:40Contributed talk (15min + 5min Q&A)
Core-collapse supernovae can synthesize $^{44}\rm Ti$ during the explosion via explosive Si-burning and $\alpha$-rich freeze-out. This radioactive isotope with a half-life of $\sim 60$ years is then observed in supernova remnants, particularly Cassiopeia A, by gamma-ray telescopes, such as the upcoming COSI mission. In this talk, I will discuss an alternative production site of $^{44}\rm Ti$...
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Dr Benjamin Wehmeyer (University of Wroclaw)27/05/2026, 10:00Contributed talk (15min + 5min Q&A)
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 neutron...
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Brian Fields (University of Illinois)28/05/2026, 09:00Invited talk (30min + 10min Q&A)
Big-bang nucleosynthesis (BBN) describes the formation of the lightest nuclides in the first minutes of cosmic time, and is a central pillar of the hot big-bang cosmology. Standard BBN combines this with the Standard Model of particle physics and nuclear cross section measurements. These allow us to make tight predictions for the primordial light element abundances, some of which are...
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Alexander Adams (Michigan State University / Facility for Rare Isotope Beams)28/05/2026, 09:40Contributed talk (15min + 5min Q&A)
Sensitivity studies have identified the $^{59}$Cu(p, $\gamma$)$^{60}$Zn and $^{59}$Cu(p, $\alpha$)$^{56}$Ni reaction rates as quantities which strongly affect the light curve and ash composition of type I X-ray bursts, and the production of $^{59}$Ni by the $\nu p$ process in supernovae. The relative rates of these reactions will determine the strength of the NiCu cycle: $^{59}$Cu(p,...
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Timothy C. Beers (University of Notre Dame)28/05/2026, 10:00Contributed talk (15min + 5min Q&A)
We present a detailed chemical-abundance analysis of an actinide-boost (log ϵ (Th/Dy) = –0.74) star, LAMOST J122216.85-063345.2 (J1222), a very metal-poor ([Fe/H] = –2.45) halo star with moderate enhancement in rapid neutron-capture (r-)process elements ([Eu/Fe] = +0.61). From high-resolution spectra (R ∼ 55,000) taken with Gemini-S/GHOST, we determine abundances for 43 elements, including...
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Falk Herwig (University of Victoria)29/05/2026, 09:00Invited talk (30min + 10min Q&A)
The intermediate neutron-capture process (i process) produces a distinct pattern of rare isotopes at neutron densities between the s and r process. Two candidate sites with predicted rapid mass ejections in the solar neighborhood are post-AGB stars undergoing very-late thermal pulses (e.g. Sakurai's object) and rapidly-accreting white dwarfs (RAWDs). Our 1D and 3D simulations show that the...
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Khang Pham (Texas A&M University)29/05/2026, 09:40Contributed talk (15min + 5min Q&A)
One aim of the upcoming Compton Spectrometer and Imager (COSI), to launch in 2027, is to measure the luminosity of gamma-rays from classical novae, presenting an exciting opportunity to constrain 18F abundance in these astrophysical phenomena. Models of classical novae have determined that nucleosynthesis and detectability of the explosion depend heavily upon the abundance of this isotope;...
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Pelagia Tsintari (Facility for Rare Isotope Beams at Michigan State University)29/05/2026, 10:00Contributed talk (15min + 5min Q&A)
The synthesis of heavy elements in explosive stellar environments, such as core-collapse supernovae, is influenced by key nuclear reactions involving unstable nuclei. In neutron-rich conditions, the α-process -a sequence of (α,xn) reactions- plays a significant part in nucleosynthesis, whereas (p,n) reactions influence element formation in proton-rich conditions, during explosive silicon...
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Dr Daid Kahl (FRIB)30/05/2026, 09:00Invited talk (30min + 10min Q&A)
Nuclear reactions frequently involve radioactive species as one or both components in explosive astrophysical scenarios, such as (super)novae, Type I X-ray bursts, and neutron star mergers. The reaction rates involved in calculating the astronomical observables are frequently unknown or poorly constrained in the Gamow window, requiring both direct and indirect measurements with both stable...
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Chirag Rathi (Texas A&M University)30/05/2026, 09:40Contributed talk (15min + 5min Q&A)
Nuclear reaction rates in stars are determined from the folding of the Maxwell Boltzmann distribution with the reaction cross section. The latter quantity describes the likelihood of interaction of two particles at a particular energy. One of the main roles of nuclear physics in the field of nuclear astrophysics is to provide information about these cross sections.
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There are many direct and... -
Thomas Stephan (University of Chicago)30/05/2026, 10:00Contributed talk (15min + 5min Q&A)
We have measured carbon, nitrogen, zirconium, molybdenum, and barium isotopes in two large presolar graphite grains found in situ in sections of the CM2 carbonaceous chondrites Murchison and Maribo. Carbon and nitrogen were analyzed using nanometer-scale secondary ion mass spectrometry (NanoSIMS), and heavy elements were measured by resonance ionization mass spectrometry (RIMS) with the...
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