Constraint of the Astrophysical $^{26g}$Al(p;γ)$^{27}$Si Destruction Rate at Stellar Temperatures
- Pain, S.D.
- Bardayan, D.W.
- Blackmon, J.C.
- Brown, S.M.
- Chae, K.Y.
- Chipps, K.A.
- Cizewski, J.A.
- Jones, K.L.
- Kozub, R.L.
- Liang, J.F.
- Matei, C.
- Matos, M.
- Moazen, B.H.
- Nesaraja, C.D.
- Okolowicz, J.
- O’Malley, P.D.
- Peters, W.A.
- Pittman, S.T.
- Ploszajczak, M.
- Schmitt, K.T.
- Shriner, J.F.
- Shapira, D.
- Smith, M.S.
- Stracener, D.W.
- Wilson, G.L.
DOIAbstract
International audienceThe Galactic 1.809-MeV γ-ray signature from the β decay of $^{26g}$Al is a dominant target of γ-rayastronomy, 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 reactionrate 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 the127-keV resonance is found to be a factor of 4 higher than the previously adopted upper ...
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