Journal
PHYSICAL REVIEW LETTERS
Volume 114, Issue 21, Pages -Publisher
AMER PHYSICAL SOC
DOI: 10.1103/PhysRevLett.114.212501
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Funding
- U.S. Department of Energy, Office of Science, Office of Nuclear Physics [DE-AC05-00OR22725, DE-FG02-96ER40955, DE-FG02-96ER40990, DE-FG02-96ER40983, DE-SC0001174]
- National Science Foundation [PHY0354870, PHY0757678]
- National Research Foundation of Korea [NRF2014S1A2A2028636]
- UK Science and Technology Facilities Council [PP/F000715/1]
- National Nuclear Security Administration under the Stewardship Science Academic Alliance program through DOE [DE-FG52-08NA28552]
- Direct For Mathematical & Physical Scien
- Division Of Physics [1067906] Funding Source: National Science Foundation
- Division Of Physics
- Direct For Mathematical & Physical Scien [1404218, 1419765] Funding Source: National Science Foundation
- Science and Technology Facilities Council [PP/F000715/1, ST/J000051/1] Funding Source: researchfish
- STFC [PP/F000715/1, ST/J000051/1] Funding Source: UKRI
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The Galactic 1.809-MeV gamma-ray signature from the beta decay of Al-26g is a dominant target of.-ray astronomy, of which a significant component is understood to originate from massive stars. The Al-26g(p,gamma)Si-27 reaction is a major destruction pathway for Al-26g at stellar temperatures, but the reaction rate is poorly constrained due to uncertainties in the strengths of low-lying resonances in Si-27. The Al-26g(d,p)Al-27 reaction has been employed in inverse kinematics to determine the spectroscopic factors, and hence resonance strengths, of proton resonances in Si-27 via mirror symmetry. The strength of the 127-keV resonance is found to be a factor of 4 higher than the previously adopted upper limit, and the upper limit for the 68-keV resonance has been reduced by an order of magnitude, considerably constraining the Al-26g destruction rate at stellar temperatures.
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