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Inverse kinematics study of the energy levels of 21Ne populated with the 20Ne +𝑑 reaction

Journal Article · · Physical Review. C
DOI:https://doi.org/10.1103/byw8-bvrn· OSTI ID:3003121
 [1];  [2];  [3];  [4];  [5];  [1];  [6];  [5];  [7];  [5];  [8];  [5];  [2];  [5];  [9]
  1. University of York (United Kingdom); TRIUMF, Vancouver, BC (Canada)
  2. University of York (United Kingdom)
  3. Argonne National Laboratory (ANL), Argonne, IL (United States); Florida State Univ., Tallahassee, FL (United States)
  4. Texas A & M Univ., College Station, TX (United States)
  5. Argonne National Laboratory (ANL), Argonne, IL (United States)
  6. University of York (United Kingdom); Univ. College London (United Kingdom)
  7. Argonne National Laboratory (ANL), Argonne, IL (United States); Los Alamos National Laboratory (LANL), Los Alamos, NM (United States)
  8. North Carolina State University, Raleigh, NC (United States); Triangle Universities Nuclear Laboratory (TUNL), Durham, NC (United States)
  9. Louisiana State Univ., Baton Rouge, LA (United States); Argonne National Laboratory (ANL), Argonne, IL (United States); UK Atomic Energy Authority (UKAEA), Culham (United Kingdom)
+ Show Author Affiliations
In recent years there has been significant experimental effort aimed at studying the impact of 16O neutron poisoning on the weak 𝑠 process in rotating massive stars. Improving the understanding of energy levels in 21Ne is crucial to reducing uncertainties in the rates of the 𝛼-induced reactions on 17O that determine the overall efficiency of the weak 𝑠 process. This paper reports on one such experiment: a study of the 20Ne (𝑑,𝑝)⁢ 21Ne reaction in inverse kinematics. Deduced spin-parity assignments were made based on adiabatic distorted-wave approximation analysis and neutron partial widths were estimated by comparison with a previous experiment. Of particular significance for nuclear astrophysics is the resulting neutron partial width for the 7820-keV energy level, estimated to be 12 200 ⁢(2900)⁢ eV, and an upper limit of ≤ 9300 eV for that of the 7749-keV energy level. These results are in tension with previous studies and therefore this paper also discusses the current state of the research into the astrophysically relevant energy levels and highlights both areas of agreement and areas of disagreement between this and various other studies that have investigated this nucleus.
Research Organization:
Duke Univ., Durham, NC (United States)
Sponsoring Organization:
USDOE Office of Science (SC), Nuclear Physics (NP)
Grant/Contract Number:
AC02-06CH11357; FG02-97ER41033
OSTI ID:
3003121
Journal Information:
Physical Review. C, Journal Name: Physical Review. C Journal Issue: 2 Vol. 112; ISSN 2469-9985; ISSN 2469-9993
Publisher:
American Physical Society (APS)Copyright Statement
Country of Publication:
United States
Language:
English

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