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Shunji NISHIMURA (RIKEN)21/09/2023, 15:45Nuclear properties for astrophysicsInvited
Where and how were heavy elements which contain many neutrons relative to proton, synthesized? With regards to the origin of these heavy elements, a reaction in which nuclei capture neutrons in a fast and continuous manner during the explosion of a star was proposed and named the rapid neutron capture process (r process) [1].
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In 2017, a binary neutron star merger event was discovered by... -
Soomi CHA (Center for Exotic Nuclear Studies, Institute for Basic Science)21/09/2023, 16:15Nuclear properties for astrophysicsOral
The $^{18}$Ne($\alpha$,$p$)$^{21}$Na reaction is one candidate of the breakout reactions from hot-CNO cycle, and it plays an important role in understanding the X-ray bursts and the nucleosynthesis in the rp-process. We investigated energy levels of the $^{22}$Mg by measuring the $\alpha$ resonant scattering on $^{18}$Ne in inverse kinematics. The $^{18}$Ne rare isotope beam was produced at...
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Max PALLÀS SOLÍS (Universitat Politècnica de Catalunya)21/09/2023, 16:30Nuclear properties for astrophysicsOral
Rapid neutron capture nucleosynthesis (the r-process) produces nearly half of the nuclei heavier than iron in explosive stellar scenarios.
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The solar system r-process residual abundances show two peaks located at $A\sim 130$ and $A\sim 195$. Between these peaks lies the Rare-Earth Peak (REP), a distinct but small peak at mass number $A\sim 160$ that arises from the freeze-out during the final... -
Thomas CHILLERY21/09/2023, 16:45Nuclear properties for astrophysicsOral
The rapid (r) neutron-capture process produces half of the elements heavier than iron and is located on the neutron-rich side of the nuclear chart. Conversely, light nuclei on the neutron-deficient side may be produced in the neutrino-driven rapid-proton capture (vp) process. Considering the r-process, promising site candidates such as core-collapse supernovae (CCSNe) and neutron star...
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Guy LECKENBY (TRIUMF)21/09/2023, 17:00Nuclear properties for astrophysicsOral
Bound-state $\beta$-decay ($\beta_b^-$-decay) is a radically transformative decay mode that can change the stability of a nucleus and generate temperature- and density-dependent decay rates. In this decay mode the $\beta$-electron is created directly in a bound atomic orbital of the daughter nucleus instead of being emitted into the continuum, so the decay channel is only significant in almost...
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Prof. G.V. ROGACHEV (Department of Physics and Astronomy, Texas A&M University)22/09/2023, 13:30Nuclear properties for astrophysicsInvited
Indirect methods play an important role in constraining the astrophysical rates of nuclear reactions. This talk will review several recent indirect studies that provided almost model-independent constraints for the key rates.
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Neutron-upscattering enhancement of the triple-alpha reaction responsible for the production of carbon, suggested in [1], was investigated by measuring a time-inverse... -
Kelly CHIPPS (Oak Ridge National Laboratory)22/09/2023, 14:00Nuclear properties for astrophysicsInvited
A variety of nucleosynthesis processes operate in our universe, producing elements across the nuclear chart. Using a range of tools and techniques, we can probe the nuclear reactions that comprise these processes. In explosive rp-process environments, direct reactions are possible using gaseous targets such as JENSA, with input from indirect techniques such as transfer reactions on both stable...
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Taka KAJINO (Beihang University/NAOJ/University of Tokyo)22/09/2023, 14:30Galactic evolutionOral
The hadronic deexcitation of the Hoyle state in 12C induced by inelastic scatterings of particles can enhance the triple-alpha reaction and the resultant accumulated seed nuclei prevent the synthesis of the heavier elements [1]. Quite recently, neutron-induced deexcitation cross sections were measured experimentally and this effect turns out to be less significant [2]. It therefore is even...
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D. KIM (Center for exotic nuclear studies, Institute Basic Science)22/09/2023, 14:45Novae and X-ray burstsOral
Knowledge of the $^{19}$Ne resonance information near the proton threshold (E$_{x}$=6.410 MeV) is important for studying the $^{18}$F($p$,$\alpha$)$^{15}$O nuclear reaction rate in a classical nova [1-4]. Several states in the vicinity of the proton threshold still have not been observed in $^{19}$Ne but were predicted by assuming isospin symmetry from its mirror state in $^{19}$F [5,6]. The...
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Hendrik Schatz (RAHUL JAIN)22/09/2023, 15:00Novae and X-ray burstsOral
I will review the current understanding of the nuclear physics of accreting neutron stars, including the rp-process and processes involving neutron rich nuclei, and their relation to observables such as X-ray bursts and the cooling of transiently accreting neutron stars. This will include new results from experiments on rp-process reactions and measurements related to crust Urca processes,...
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Yi Hua LAM (Institute of Modern Physics, Chinese Academy of Sciences)Nuclear properties for astrophysicsOral
We use the type-I X-ray burst models, constructed by the one-dimensional multi-zone hydrodynamic KEPLER code [1], and complying with the burst light curves and recurrence times of the observed GS 1826−24 clocked bursts and SAX J1808.4−3658 photospheric radius expansion (PRE) bursts to investigate the combined impact of the latest 22Mg(α,p)25Al [2], 56Ni(p,γ)57Cu [3], 57Cu(p,γ)58Zn [4],...
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