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Gao, B; Giraud, S; Li, K A; Sieverding, A; Zegers, R G T; Tang, X; Ash, J; Ayyad-Limonge, Y; Bazin, D; Biswas, S; Brown, B A; Chen, J; DeNudt, M; Farris, P; Gabler, J M; Gade, A; Ginter, T; Grinder, M; Heger, A; Hultquist, C; Hill, A M; Iwasaki, H; Kwan, E; Li, J; Longfellow, B; Maher, C; Ndayisabye, F; Noji, S; Pereira, J; Qi, C; Rebenstock, J; Revel, A; Rhodes, D; Sanchez, A; Schmitt, J; Sumithrarachchi, C; Sun, B H; Weisshaar, D.
Affiliation
  • Gao B; CAS Key Laboratory of High Precision Nuclear Spectroscopy, Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou 73000, People's Republic of China.
  • Giraud S; School of Nuclear Science and Technology, University of Chinese Academy of Sciences, Beijing 100049, People's Republic of China.
  • Li KA; National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA.
  • Sieverding A; CAS Key Laboratory of High Precision Nuclear Spectroscopy, Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou 73000, People's Republic of China.
  • Zegers RGT; School of Nuclear Science and Technology, University of Chinese Academy of Sciences, Beijing 100049, People's Republic of China.
  • Tang X; School of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota 55455, USA.
  • Ash J; National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA.
  • Ayyad-Limonge Y; Joint Institute for Nuclear Astrophysics-Center for the Evolution of the Elements, Michigan State University, East Lansing, Michigan 48824, USA.
  • Bazin D; Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA.
  • Biswas S; CAS Key Laboratory of High Precision Nuclear Spectroscopy, Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou 73000, People's Republic of China.
  • Brown BA; School of Nuclear Science and Technology, University of Chinese Academy of Sciences, Beijing 100049, People's Republic of China.
  • Chen J; National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA.
  • DeNudt M; Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA.
  • Farris P; National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA.
  • Gabler JM; National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA.
  • Gade A; Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA.
  • Ginter T; National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA.
  • Grinder M; National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA.
  • Heger A; Joint Institute for Nuclear Astrophysics-Center for the Evolution of the Elements, Michigan State University, East Lansing, Michigan 48824, USA.
  • Hultquist C; Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA.
  • Hill AM; National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA.
  • Iwasaki H; National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA.
  • Kwan E; Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA.
  • Li J; National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA.
  • Longfellow B; Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA.
  • Maher C; National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA.
  • Ndayisabye F; National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA.
  • Noji S; Joint Institute for Nuclear Astrophysics-Center for the Evolution of the Elements, Michigan State University, East Lansing, Michigan 48824, USA.
  • Pereira J; Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA.
  • Qi C; National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA.
  • Rebenstock J; National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA.
  • Revel A; Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA.
  • Rhodes D; School of Physics and Astronomy, Monash University, Victoria 3800, Australia.
  • Sanchez A; National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA.
  • Schmitt J; Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA.
  • Sumithrarachchi C; National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA.
  • Sun BH; Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA.
  • Weisshaar D; National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA.
Phys Rev Lett ; 126(15): 152701, 2021 Apr 16.
Article in En | MEDLINE | ID: mdl-33929230
ABSTRACT
The discrepancy between observations from γ-ray astronomy of the ^{60}Fe/^{26}Al γ-ray flux ratio and recent calculations is an unresolved puzzle in nuclear astrophysics. The stellar ß-decay rate of ^{59}Fe is one of the major nuclear uncertainties impeding us from a precise prediction. The important Gamow-Teller strengths from the low-lying states in ^{59}Fe to the ^{59}Co ground state are measured for the first time using the exclusive measurement of the ^{59}Co(t,^{3}He+γ)^{59}Fe charge-exchange reaction. The new stellar decay rate of ^{59}Fe is a factor of 3.5±1.1 larger than the currently adopted rate at T=1.2 GK. Stellar evolution calculations show that the ^{60}Fe production yield of an 18 solar mass star is decreased significantly by 40% when using the new rate. Our result eliminates one of the major nuclear uncertainties in the predicted yield of ^{60}Fe and alleviates the existing discrepancy of the ^{60}Fe/^{26}Al ratio.
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Full text: 1 Collection: 01-internacional Database: MEDLINE Type of study: Prognostic_studies Language: En Journal: Phys Rev Lett Year: 2021 Document type: Article
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Full text: 1 Collection: 01-internacional Database: MEDLINE Type of study: Prognostic_studies Language: En Journal: Phys Rev Lett Year: 2021 Document type: Article