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Informing direct neutron capture on tin isotopes near the N=82 shell closure

Journal Article · · Physical Review C
 [1];  [2];  [3];  [4];  [5];  [6];  [7];  [8];  [9];  [3];  [10];  [6];  [11];  [6];  [12];  [13];  [6];  [14];  [15];  [3] more »;  [10];  [6];  [6];  [12] « less
  1. Rutgers Univ., New Brunswick, NJ (United States). Dept. of Physics and Astronomy; Los Alamos National Lab. (LANL), Los Alamos, NM (United States). Physics Division
  2. Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States). Reactor and Nuclear Systems Division
  3. Rutgers Univ., New Brunswick, NJ (United States). Dept. of Physics and Astronomy
  4. Tennessee Technological Univ., Cookeville, TN (United States). Dept. of Physics
  5. Univ. of Tennessee, Knoxville, TN (United States). Dept. of Physics and Astronomy; Michigan State Univ., East Lansing, MI (United States). Dept. of Physics and Astronomy, and JINA-CEE
  6. Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States). Physics Division
  7. Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States). Physics Division; Univ. of Notre Dame, IN (United States). Dept. of Physics
  8. Sungkyunkwan Univ., Suwon (Republic of Korea). Dept. of Physics
  9. Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States). Physics Division; Colorado School of Mines, Golden, CO (United States). Dept. of Physics
  10. Univ. of Tennessee, Knoxville, TN (United States). Dept. of Physics and Astronomy
  11. Louisiana State Univ., Baton Rouge, LA (United States). Dept. of Physics and Astronomy
  12. Michigan State Univ., East Lansing, MI (United States). Dept. of Physics and Astronomy
  13. Rutgers Univ., New Brunswick, NJ (United States). Dept. of Physics and Astronomy; Univ. of Notre Dame, IN (United States). Dept. of Physics
  14. Oak Ridge Associated Univ., Oak Ridge, TN (United States)
  15. Univ. of Tennessee, Knoxville, TN (United States). Dept. of Physics and Astronomy; Oak Ridge Associated Univ., Oak Ridge, TN (United States)
Half of the elements heavier than iron are believed to be produced through the rapid neutron-capture process ($$r$$-process). The astrophysical environment(s) where the $$r$$-process occurs remains an open question, even after recent observations of neutron-star mergers and the associated kilonova. Features in the abundance pattern of $$r$$-process ashes may provide critical insight for distinguishing contributions from different possible sites, including neutron-star mergers and core-collapse supernovae. In particular, the largely unknown neutron-capture reaction rates on neutron-rich unstable nuclei near 132Sn could have a significant impact on the final $$r$$-process abundances. To better determine these neutron-capture rates, the ($d,p$) reaction has been measured in inverse kinematics using radioactive ion beams of 126Sn and 128Sn and a stable beam of 124Sn interacting with a (CD2)$$_n$$ target. An array of position-sensitive silicon strip detectors, including the Super Oak Ridge Rutgers University Barrel Array, was used to detect light reaction products. In addition to the present measurements, previous measurements of 130,132Sn($d,p$) were reanalyzed using state-of-the-art reaction theory to extract a consistent set of spectroscopic factors for ($d,p$) reactions on even tin nuclei between the heaviest stable isotope 124Sn and doubly magic 132Sn. The spectroscopic information was used to calculate direct-semidirect ($n,γ$) cross sections, which will serve as important input for r-process abundance calculations.
Research Organization:
Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States)
Sponsoring Organization:
USDOE; USDOE Office of Science (SC)
Grant/Contract Number:
AC05-00OR22725; FG02-96ER40955; FG02-96ER40983; FG52-08NA28552; NA0002132; SC0001174
OSTI ID:
1564107
Alternate ID(s):
OSTI ID: 1507606
Journal Information:
Physical Review C, Journal Name: Physical Review C Journal Issue: 4 Vol. 99; ISSN PRVCAN; ISSN 2469-9985
Publisher:
American Physical Society (APS)Copyright Statement
Country of Publication:
United States
Language:
English

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