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Abstract / Description of output
In Wolf-Rayet and asymptotic giant branch (AGB) stars, the 26gAl(p,γ)27Si reaction is expected to govern the destruction of the cosmic γ-ray emitting nucleus 26Al. The rate of this reaction, however, is highly uncertain due to the unknown properties of key resonances in the temperature regime of hydrogen burning. We present a high-resolution inverse kinematic study of the 26gAl(d,p)27Al reaction as a method for constraining the strengths of key astrophysical resonances in the 26gAl(p,γ)27Si reaction. In particular, the results indicate that the resonance at Er=127 keV in 27Si determines the entire 26gAl(p,γ)27Si reaction rate over almost the complete temperature range of Wolf-Rayet stars and AGB stars.
Keywords / Materials (for Non-textual outputs)
- EARLY SOLAR-SYSTEM
- MASSIVE STARS
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- 1 Finished
1/08/11 → 31/07/15