Informing direct neutron capture on tin isotopes near the shell closure
Abstract
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.
- Authors:
-
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- Rutgers Univ., New Brunswick, NJ (United States). Dept. of Physics and Astronomy; Los Alamos National Lab. (LANL), Los Alamos, NM (United States). Physics Division
- Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States). Reactor and Nuclear Systems Division
- Rutgers Univ., New Brunswick, NJ (United States). Dept. of Physics and Astronomy
- Tennessee Technological Univ., Cookeville, TN (United States). Dept. of Physics
- 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
- Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States). Physics Division
- Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States). Physics Division; Univ. of Notre Dame, IN (United States). Dept. of Physics
- Sungkyunkwan Univ., Suwon (Republic of Korea). Dept. of Physics
- Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States). Physics Division; Colorado School of Mines, Golden, CO (United States). Dept. of Physics
- Univ. of Tennessee, Knoxville, TN (United States). Dept. of Physics and Astronomy
- Louisiana State Univ., Baton Rouge, LA (United States). Dept. of Physics and Astronomy
- Michigan State Univ., East Lansing, MI (United States). Dept. of Physics and Astronomy
- Rutgers Univ., New Brunswick, NJ (United States). Dept. of Physics and Astronomy; Univ. of Notre Dame, IN (United States). Dept. of Physics
- Oak Ridge Associated Univ., Oak Ridge, TN (United States)
- Univ. of Tennessee, Knoxville, TN (United States). Dept. of Physics and Astronomy; Oak Ridge Associated Univ., Oak Ridge, TN (United States)
- Publication Date:
- Research Org.:
- Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC)
- OSTI Identifier:
- 1564107
- Alternate Identifier(s):
- OSTI ID: 1507606
- Grant/Contract Number:
- AC05-00OR22725; FG52-08NA28552; NA0002132; FG02-96ER40983; SC0001174; FG02-96ER40955
- Resource Type:
- Accepted Manuscript
- Journal Name:
- Physical Review C
- Additional Journal Information:
- Journal Volume: 99; Journal Issue: 4; Journal ID: ISSN 2469-9985
- Publisher:
- American Physical Society (APS)
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 73 NUCLEAR PHYSICS AND RADIATION PHYSICS
Citation Formats
Manning, B., Arbanas, G., Cizewski, J. A., Kozub, R. L., Ahn, S., Allmond, J. M., Bardayan, D. W., Chae, K. Y., Chipps, K. A., Howard, M. E., Jones, K. L., Liang, J. F., Matos, M., Nesaraja, C. D., Nunes, F. M., O'Malley, P. D., Pain, S. D., Peters, W. A., Pittman, S. T., Ratkiewicz, A., Schmitt, K. T., Shapira, D., Smith, M. S., and Titus, L. Informing direct neutron capture on tin isotopes near the N=82 shell closure. United States: N. p., 2019.
Web. doi:10.1103/PhysRevC.99.041302.
Manning, B., Arbanas, G., Cizewski, J. A., Kozub, R. L., Ahn, S., Allmond, J. M., Bardayan, D. W., Chae, K. Y., Chipps, K. A., Howard, M. E., Jones, K. L., Liang, J. F., Matos, M., Nesaraja, C. D., Nunes, F. M., O'Malley, P. D., Pain, S. D., Peters, W. A., Pittman, S. T., Ratkiewicz, A., Schmitt, K. T., Shapira, D., Smith, M. S., & Titus, L. Informing direct neutron capture on tin isotopes near the N=82 shell closure. United States. https://doi.org/10.1103/PhysRevC.99.041302
Manning, B., Arbanas, G., Cizewski, J. A., Kozub, R. L., Ahn, S., Allmond, J. M., Bardayan, D. W., Chae, K. Y., Chipps, K. A., Howard, M. E., Jones, K. L., Liang, J. F., Matos, M., Nesaraja, C. D., Nunes, F. M., O'Malley, P. D., Pain, S. D., Peters, W. A., Pittman, S. T., Ratkiewicz, A., Schmitt, K. T., Shapira, D., Smith, M. S., and Titus, L. Thu .
"Informing direct neutron capture on tin isotopes near the N=82 shell closure". United States. https://doi.org/10.1103/PhysRevC.99.041302. https://www.osti.gov/servlets/purl/1564107.
@article{osti_1564107,
title = {Informing direct neutron capture on tin isotopes near the N=82 shell closure},
author = {Manning, B. and Arbanas, G. and Cizewski, J. A. and Kozub, R. L. and Ahn, S. and Allmond, J. M. and Bardayan, D. W. and Chae, K. Y. and Chipps, K. A. and Howard, M. E. and Jones, K. L. and Liang, J. F. and Matos, M. and Nesaraja, C. D. and Nunes, F. M. and O'Malley, P. D. and Pain, S. D. and Peters, W. A. and Pittman, S. T. and Ratkiewicz, A. and Schmitt, K. T. and Shapira, D. and Smith, M. S. and Titus, L.},
abstractNote = {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.},
doi = {10.1103/PhysRevC.99.041302},
journal = {Physical Review C},
number = 4,
volume = 99,
place = {United States},
year = {Thu Apr 18 00:00:00 EDT 2019},
month = {Thu Apr 18 00:00:00 EDT 2019}
}
Web of Science
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