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Observation of Doppler broadening in β-delayed proton-γ decay

S. B. Schwartz, C. Wrede, M. B. Bennett, S. N. Liddick, D. Pérez-Loureiro, A. Bowe, A. A. Chen, K. A. Chipps, N. Cooper, D. Irvine, E. McNeice, F. Montes, F. Naqvi, R. Ortez, S. D. Pain, J. Pereira, C. Prokop, J. Quaglia, S. J. Quinn, J. Sakstrup, M. Santia, S. Shanab, A. Simon, A. Spyrou, and E. Thiagalingam
Phys. Rev. C 92, 031302(R) – Published 14 September 2015

Abstract

Background: The Doppler broadening of γ-ray peaks due to nuclear recoil from β-delayed nucleon emission can be used to measure the energies of the nucleons. This method has never been tested using β-delayed proton emission or applied to a recoil heavier than A=10.

Purpose: To test and apply this Doppler broadening method using γ-ray peaks from the P26(βpγ)Al25 decay sequence.

Methods: A fast beam of P26 was implanted into a planar Ge detector, which was used as a P26 β-decay trigger. The SeGA array of high-purity Ge detectors was used to detect γ rays from the P26(βpγ)Al25 decay sequence.

Results: Radiative Doppler broadening in β-delayed proton-γ decay was observed for the first time. The Doppler broadening analysis method was verified using the 1613-keV γ-ray line for which the proton energies were previously known. The 1776-keV γ ray de-exciting the 2720 keV Al25 level was observed in P26(βpγ)Al25 decay for the first time and used to determine that the center-of-mass energy of the proton emission feeding the 2720-keV level is 5.1±1.0 (stat.) ±0.6 (syst.) MeV, corresponding to a Si26 excitation energy of 13.3±1.0 (stat.) ±0.6 (syst.) MeV for the proton-emitting level.

Conclusions: The Doppler broadening method has been demonstrated to provide practical measurements of the energies for β-delayed nucleon emissions populating excited states of nuclear recoils at least as heavy as A=25.

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  • Received 24 July 2015

DOI:https://doi.org/10.1103/PhysRevC.92.031302

©2015 American Physical Society

Authors & Affiliations

S. B. Schwartz1,2,3,*, C. Wrede1,2,†, M. B. Bennett1,2, S. N. Liddick4,2, D. Pérez-Loureiro2, A. Bowe1,2,5, A. A. Chen6, K. A. Chipps7,8,9, N. Cooper10, D. Irvine6, E. McNeice6, F. Montes2,11, F. Naqvi10, R. Ortez1,2,12, S. D. Pain8, J. Pereira2,11, C. Prokop4,2, J. Quaglia13,11,2, S. J. Quinn1,2,11, J. Sakstrup1,2, M. Santia1,2, S. Shanab1,2, A. Simon2,14, A. Spyrou1,2,11, and E. Thiagalingam6

  • 1Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA
  • 2National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
  • 3Geology and Physics Department, University of Southern Indiana, Evansville, Indiana 47712, USA
  • 4Department of Chemistry, Michigan State University, East Lansing, Michigan 48824, USA
  • 5Physics Department, Kalamazoo College, Kalamazoo, Michigan 49006, USA
  • 6Department of Physics and Astronomy, McMaster University, Hamilton, Ontario L8S 4M1, Canada
  • 7Department of Physics, Colorado School of Mines, Golden, Colorado 08401, USA
  • 8Physics Division, Oak Ridge National Laboratory, Oak Ridge, Tennessee 37831, USA
  • 9Department of Physics and Astronomy, University of Tennessee, Knoxville, Tennessee 37996, USA
  • 10Department of Physics and Wright Nuclear Structure Laboratory, Yale University, New Haven, Connecticut 06520, USA
  • 11Joint Institute for Nuclear Astrophysics, Michigan State University, East Lansing, Michigan 48824, USA
  • 12Department of Physics, University of Washington, Seattle, Washington 98195, USA
  • 13Department of Electrical Engineering, Michigan State University, East Lansing, Michigan 48824, USA
  • 14Department of Physics and Joint Institute for Nuclear Astrophysics, University of Notre Dame, Notre Dame, Indiana 46556, USA

  • *schwartz@nscl.msu.edu
  • wrede@nscl.msu.edu

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Vol. 92, Iss. 3 — September 2015

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