12C(α,γ)16O:: The key reaction in stellar nucleosynthesis
12C(α,γ)16O:: The key reaction in stellar nucleosynthesis
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DOI：
10.1103/physrevlett.863244
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发表时间：
2001-04-09
影响因子：
8.6
通讯作者：
Paradellis, T
中科院分区：
文献类型：
--
作者：
Kunz, R;Jaeger, M;Paradellis, T
在E-cm=0.95-2.8 MeV的能量范围内，在20个能点测量了C-12(α，γ)O-16反应产生的伽马射线的角分布。与以前的直接调查相比，本实验的灵敏度提高了1-2个数量级，使用了由BGO主动屏蔽的高效(100%)Ge探测器阵列，以及由斯图加特DYNAMITRON加速器提供的高达500微安的束流。由伽马角分布导出的Se_1和Se_2因子用R-矩阵方法外推到氦燃烧温度范围内，得到S-E_1(300)=(76+/-20)keV_b和S-E_2(300)=(85+/-30)keV_b。
The angular distributions of gamma rays from the C-12(alpha, gamma)O-16 reaction have been measured at 20 energy points in the energy range E-cm = 0.95 to 2.8 MeV. The sensitivity of the present experiment compared to previous direct investigations was raised by 1-2 orders of magnitude, by using an array of highly efficient (100%) Ge detectors shielded actively with BGOs, as well as high beam currents of up to 500 muA that were provided by the Stuttgart DYNAMITRON accelerator. The SE1 and SE2 factors deduced from the gamma angular distributions have been extrapolated to the range of helium burning temperatures applying the R-matrix method, which yielded S-E1(300) = (76 +/- 20) keV b and S-E2(300) = (85 +/- 30) keV b.