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Constraint of the Astrophysical $^{26g}$Al(p;γ)$^{27}$Si Destruction Rate at Stellar Temperatures

Abstract : The Galactic 1.809-MeV γ-ray signature from the β decay of $^{26g}$Al is a dominant target of γ-ray astronomy, of which a significant component is understood to originate from massive stars. The $^{26g}$Al(p; γ)$^{27}$Si reaction is a major destruction pathway for $^{26g}$Al at stellar temperatures, but the reaction rate is poorly constrained due to uncertainties in the strengths of low-lying resonances in $^{27}$Si. The $^{26g}$Al(d; p)$^{27}$Al reaction has been employed in inverse kinematics to determine the spectroscopic factors, and hence resonance strengths, of proton resonances in $^{27}$Si 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 $^{26g}$Al destruction rate at stellar temperatures.
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Contributor : Michel Lion Connect in order to contact the contributor
Submitted on : Monday, June 1, 2015 - 8:55:48 AM
Last modification on : Friday, January 21, 2022 - 9:30:17 AM

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S.D. Pain, D.W. Bardayan, J.C. Blackmon, S.M. Brown, K.Y. Chae, et al.. Constraint of the Astrophysical $^{26g}$Al(p;γ)$^{27}$Si Destruction Rate at Stellar Temperatures. Physical Review Letters, American Physical Society, 2015, 114 (21), pp.212501. ⟨10.1103/PhysRevLett.114.212501⟩. ⟨in2p3-01158394⟩



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