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Constraints for stellar electron-capture rates on 86Kr via the 86Kr(t, 3He +γ) 86Br reaction and the implications for core-collapse supernovae

Journal Article · · Physical Review C
 [1];  [2];  [1];  [3];  [4];  [5];  [1];  [6];  [3];  [2];  [1];  [7];  [4];  [1];  [3];  [3];  [4];  [8];  [8];  [1] more »;  [1];  [4];  [9] « less
  1. Michigan State Univ., East Lansing, MI (United States). National Superconducting Cyclotron Lab.; Michigan State Univ., East Lansing, MI (United States). Joint Institute for Nuclear Astrophysics - Center for the Evolution of the Elements; Michigan State Univ., East Lansing, MI (United States). Dept. of Physics and Astronomy
  2. Univ. of North Carolina, Chapel Hill, NC (United States). Dept. of Physics and Astronomy
  3. Michigan State Univ., East Lansing, MI (United States). National Superconducting Cyclotron Lab.; Michigan State Univ., East Lansing, MI (United States). Dept. of Physics and Astronomy
  4. Michigan State Univ., East Lansing, MI (United States). National Superconducting Cyclotron Lab.
  5. Univ. of Massachusetts, Lowell, MA (United States). Dept. of Physics
  6. Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
  7. Chinese Academy of Sciences (CAS), Lanzhou (China). Institute of Modern Physics
  8. Michigan State Univ., East Lansing, MI (United States). National Superconducting Cyclotron Lab.; Michigan State Univ., East Lansing, MI (United States). Joint Institute for Nuclear Astrophysics - Center for the Evolution of the Elements
  9. Univ. of Sao Paulo (Brazil). Instituto di Fisica
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Background: In the late stages of stellar core collapse just prior to core bounce, electron captures on medium-heavy nuclei drive deleptonization. Therefore, simulations require the use of accurate reaction rates. Nuclei with neutron number near N=50 above atomic number Z=28 play an important role. Rates presently used in astrophysical simulations rely primarily on a relatively simple single-state approximation. In order to improve the accuracy of the astrophysical simulations, experimental data are needed to test the electron-capture rates and to guide the development of better theoretical models and astrophysical simulations. Purpose: The purpose of the present work was to measure the Gamow-Teller transition strength from 86Kr to 86Br, to derive the stellar electron-capture rates based on the extracted strengths, and to compare the derived rates with rates based on shell-model and quasiparticle random-phase approximation (QRPA) Gamow-Teller strengths calculations, as well as the single-state approximation. An additional purpose was to test the impact of using improved electron-capture rates on the late evolution of core-collapse supernovae. Method: The Gamow-Teller strengths from 86Kr were extracted from the 86Kr(t, 3He +γ) charge-exchange reaction at 115MeV/u. The electron-capture rates were calculated as a function of stellar density and temperature. Besides the case of 86Kr, the electron-capture rates based on the QRPA calculations were calculated for 78 additional isotopes near N=50 above Z=28. The impact of using these rates instead of those based on the single-state approximation is studied in a spherically symmetrical simulation of core collapse just prior to bounce. Results: The derived electron-capture rates on 86Kr from the experimental Gamow-Teller strength distribution are much smaller than the rates estimated based on the single-state approximation. Rates based on Gamow-Teller strengths estimated in shell-model and QRPA calculations are more accurate. The core-collapse supernova simulation with electron-capture rates based on the QRPA calculations indicate a significant reduction in the deleptonization during the collapse phase. Conclusions: It is important to utilize microscopic theoretical models that are tested by experimental data to constrain and estimate Gamow-Teller strengths and derived electron-capture rates for nuclei near N=50 that are inputs for astrophysical simulations of core-collapse supernovae and their multimessenger signals, such as the emission of neutrinos and gravitational waves.
Research Organization:
Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States)
Sponsoring Organization:
USDOE Office of Science (SC)
Grant/Contract Number:
AC02-05CH11231
OSTI ID:
1782131
Journal Information:
Physical Review C, Journal Name: Physical Review C Journal Issue: 4 Vol. 100; ISSN 2469-9985
Publisher:
American Physical Society (APS)Copyright Statement
Country of Publication:
United States
Language:
English

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Cited By (3)

Gamow-Teller transitions to Zr 93 via the Nb 93 ( t , He 3 + γ ) reaction at 115 MeV/u and its application to the stellar electron-capture rates journal January 2020
Impact of electron capture rates for nuclei far from stability on core-collapse supernovae journal January 2020
Impact of electron capture rates on nuclei far from stability on core-collapse supernovae text January 2019

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