Spillane T, Raiola F, Rolfs C, Schürmann D, Strieder F, Zeng S, Becker H-W, Bordeanu C, Gialanella L, Romano M, Schweitzer J
University of Connecticut, Storrs, Connecticut, USA.
Phys Rev Lett. 2007 Mar 23;98(12):122501. doi: 10.1103/PhysRevLett.98.122501. Epub 2007 Mar 21.
The fusion reactions 12C(12C,alpha)20Ne and 12C(12C,p)23Na have been studied from E=2.10 to 4.75 MeV by gamma-ray spectroscopy using a C target with ultralow hydrogen contamination. The deduced astrophysical S(E)* factor exhibits new resonances at E< or =3.0 MeV, in particular, a strong resonance at E=2.14 MeV, which lies at the high-energy tail of the Gamow peak. The resonance increases the present nonresonant reaction rate of the alpha channel by a factor of 5 near T=8x10(8) K. Because of the resonance structure, extrapolation to the Gamow energy EG=1.5 MeV is quite uncertain. An experimental approach based on an underground accelerator placed in a salt mine in combination with a high efficiency detection setup could provide data over the full EG energy range.
利用具有超低氢污染的碳靶，通过伽马射线光谱法对能量范围为E = 2.10至4.75兆电子伏的聚变反应12C(12C,α)20Ne和12C(12C,p)23Na进行了研究。推导得出的天体物理S(E)*因子在E≤3.0兆电子伏处呈现出新的共振，特别是在E = 2.14兆电子伏处有一个强共振，该共振位于伽莫夫峰的高能尾部。在T = 8×10⁸K附近，该共振使α通道当前的非共振反应速率提高了5倍。由于共振结构，外推至伽莫夫能量EG = 1.5兆电子伏存在相当大的不确定性。一种基于放置在盐矿中的地下加速器并结合高效探测装置的实验方法，能够在整个EG能量范围内提供数据。
