13C(α,n)16O是慢中子俘获过程(s-过程)的主要中子源反应。由于存在阈下共振，而且高能区现有实验数据存在分歧，该反应在天体物理能区的反应截面有较大不确定性，影响我们对重元素核合成的理解。为了解决这一问题，我们将利用四川大学的3MV串列静电加速器和锦屏深地核天体物理(JUNA)团队研发的低本底高灵敏度中子探测器，对13C(α,n)16O反应截面进行直接测量。实验将结合(p,γ)与背散射(RBS)测量13C靶厚；利用D(d,n)反应对JUNA的中子探测器进行效率刻度；并在质心系能量Ecm=0.35-1.5 MeV范围内测量13C(α,n)16O反应截面，去除高能区实验数据的分歧。实验测量能区将与锦屏深地实验室能区(0.2-0.31 MeV)形成互补，得到完整实验数据，约束理论模型外推，为天体物理研究提供可靠的反应率。

The 13C(α,n)16O reaction is the key neutron source reaction for the stellar s-process nucleosynthesis. Due to the existence of sub-threshold resonances and disagreements of the existing data at higher energy, there is a rather large uncertainty in this important reaction rate which limits our understanding to the nucleosynthesis of heavy elements. We will take the advantage of the new 3MV tandetron accelerator in Sichuan University and high sensitive neutron detector of Jinping Underground lab for Nuclear Astrophysics (JUNA) to study this important reaction. We will cross check the thickness of thin 13C target by (p,γ) reaction and Rutherford backscattering, then apply D(d,n) reaction to calibrate the efficiency of JUNA neutron detector and finally measure the 13C(α,n)16O reaction cross section at center of mass energy range 0.35-1.5 MeV to eliminate the disagreement in the existing data. Our energy range is complementary to that of JUNA project. Together with JUNA measurement, our results will improve the predictive power of extrapolating model, providing a reliable astrophysical reaction rate, and eliminating one important uncertainty in stellar nucleosynthesis model.