A5031087649- Nuclear physics research studies
- Nuclear Physics and Applications
- Radiation Detection and Scintillator Technologies
- Astro and Planetary Science
- X-ray Spectroscopy and Fluorescence Analysis
- Particle Detector Development and Performance
- Particle physics theoretical and experimental studies
- Gamma-ray bursts and supernovae
- Atomic and Molecular Physics
- Nuclear reactor physics and engineering
- Astronomical and nuclear sciences
- Rare-earth and actinide compounds
- Astrophysical Phenomena and Observations
- Mass Spectrometry Techniques and Applications
- High-pressure geophysics and materials
- Neutrino Physics Research
- Advanced NMR Techniques and Applications
- Scientific Research and Discoveries
- Radiation Therapy and Dosimetry
Chinese Academy of Sciences
2020-2023
Institute of Modern Physics
2020-2023
University of Chinese Academy of Sciences
2020-2023
The ^{13}C(α,n)^{16}O reaction is the main neutron source for slow-neutron-capture process in asymptotic giant branch stars and intermediate process. Direct measurements at astrophysical energies above-ground laboratories are hindered by extremely small cross sections vast cosmic-ray-induced background. We performed first consistent direct measurement range of E_{c.m.}=0.24 to 1.9 MeV using accelerators China Jinping Underground Laboratory Sichuan University. Our covers almost entire Gamow...
The ^{18}O(α,γ)^{22}Ne reaction is critical for AGB star nucleosynthesis due to its connection the abundances of several key isotopes, such as ^{21}Ne and ^{22}Ne. However, ambiguous resonance energy spin-parity dominant 470 keV leads substantial uncertainty in rate temperature interest. We have measured energies strengths low-energy resonances at Jinping Underground Nuclear Astrophysics experimental facility (JUNA) with improved precision. has been be E_{α}=474.0±1.1 keV, high precision...
The carbon fusion reaction is crucial in stellar evolution. Despite six decades of studies, there still a large uncertainty the rate which limits our understanding various objects, such as massive stars, type Ia supernovae, and superbursts. In this paper, we review experimental theoretical studies at sub-barrier energies. An outlook for future also presented.
We report the first (in)elastic scattering measurement of ^{25}Al+p with capability to select and measure in a broad energy range proton resonances ^{26}Si contributing ^{22}Mg(α,p) reaction at type I x-ray burst energies. measured spin-parities four above α threshold that are found strongly impact rate. The new rate advances state-of-the-art model remarkably reproduce light curves GS 1826-24 clocked burster mean deviation <9% permits us discover strong correlation between He abundance...
The $^{16}\mathrm{F}$ nucleus is situated at the proton drip line and unbound by emission only about 500 keV. Continuum coupling then prominent in this nucleus. Added to that, its low-lying spectrum consists of narrow resonances as well. It therefore a very good candidate study nuclear structure reactions line. scattering proton-proton cross section were calculated with coupled-channels Gamow shell model framework case using an effective Hamiltonian. Experimental data are well reproduced,...
Abstract The 12 C+ C fusion reaction plays a crucial role in stellar evolution and explosions. Its main open channels include , p n 8 Be. Despite more than half century of efforts, large differences remain among the experimental data this measured using various techniques. In work, we analyze existing statistical model. Our calculation shows following: 1) relative systematic uncertainties predicted branching ratios decrease as increase; 2) total modified astrophysical S -factors ( * factors)...
Abstract The 12 C+ C fusion reaction was studied in the range of E c.m. =8.9 to 21 MeV using active-target Time Projection Chamber. With full information on all tracks products, cross sections C( C, 8 Be) 16 O g.s. channel and C,3 α ) could be measured down level a few milibarns. determined 10 mb at =11.1 MeV, supporting direct transfer mechanism. for first time an exclusive measurement. Our result does not confirm anomaly behavior reported previous inclusive measurement by Kolata et al ....
Abstract The 18 O( p , α ) 15 N reaction is of particular importance for influencing the abundances key isotopes such as 19 F, O, and N. Peculiar these nuclei are observed from spectra or meteorite grains originating in asymptotic giant branch stars. could provide a way to explain discrepancy between observations model predictions. A comprehensive R -matrix analysis has been performed by including additional constraints other channels; particular, N+ scattering data were involved first time....
The strength of the narrow resonance $^{13}\mathrm{C}(\ensuremath{\alpha},n)^{16}\mathrm{O}$ reaction at ${E}_{\ensuremath{\alpha}}=1055.63$ keV is determined to be $16.9\ifmmode\pm\else\textpm\fi{}0.4(\mathrm{stat})\ifmmode\pm\else\textpm\fi{}1.7(\text{sys})$ eV. and cross section in vicinity are used reconcile inconsistencies past measurements. Our normalization factors agree with recommendation ENDF/B-VIII.0 evaluation CIELO project. sum strengths two resonances around...
Astrophysical reactions involving radioactive isotopes (RI) often play an important role in high-temperature stellar environments. The experimental studies on the reaction rates for those are still limited mainly due to technical difficulties producing high-quality RI beams. A direct measurement of would be challenging many cases, however, we can make a reliable evaluation by indirect method or studying resonance prorerties. Here ntroduce recent examples such RI-involving astrophysical...
Type I X-ray bursts (XRBs) are the most frequently observed thermonuclear explosions in nature. The 22 Mg( α ,p) 25 Al reaction plays a critical role XRB models. However, experimental information is insufficient to deduce precise rate for respective temperature range. A new measurement of Al+p resonant scattring was performed up astrophysically interested energy region Al. Several resonances were excitation functions, and their level properties have been determined based on an R-matrix...
Experimental studies on astrophysical reactions involving radioactive isotopes (RI) often accompany technical challenges. Studies such nuclear have been conducted at the low-energy RI beam separator CRIB, operated by Center for Nuclear Study, University of Tokyo. We discuss two cases reaction CRIB; one is 7 Be+ n which may affect primordial Li abundance in Big-Bang nucleosynthesis, and other 22 Mg( α , p ) relevantin X-raybursts.
A low-background neutron detector array was developed to measure the cross section of $^{13}$C($\alpha$,n)$^{16}$O reaction, which is source for $s$-process in AGB stars, Gamow window ($E_{c.m.}$ = 190 $\pm$ 40 keV) at China Jinping Underground Laboratory (CJPL). The consists 24 $^{3}$He proportional counters embedded a polyethylene cube. Due deep underground location and borated shield around array, low background 4.5(2)/hour achieved. $^{51}$V(p, n)$^{51}$Cr reaction used determine...