Determination of Astrophysical ~(26)Si(p, γ)~(27)P Reaction Rate From Asymptotic Normalization Coefficients of ~(27)Mg → ~(26)Mg n

The 1.809 MeV γ-ray from the decay of 26Al is an excellent observable for some astrophysical events, such as novae and X-ray burst. The nucleosynthesis of 26Al is dominated by the reaction chain 24Mg(p,γ)25Al(β )25Mg(p,γ)26Al, however, it is complicat…     

Measurement of ^17F（d,n）^18Ne Reaction

Explosive hydrogen burning occurs in very massive （M≥ 10^5-10^8 M） star with high temperature and density. Hot pp chain, hot CNO, hot NeNa-MgAl chain and the flowing γp and ap process will play a prominent role in hydrogen burning as. the temperature goes higher. When the temperature of the star is hither than 10^8 K. high temnerature CNO chain is dominant in hydrogen burning,     

Theoretical Study of ^2H（d,γ）^4He Reaction Below Ecm〈3 MeV

The reaction cross sections of ^2H（d,γ）^4He at the astrophysically interesting energies （about below few hundreds of keV） are extremely low. Presently it is impractical to measure in the laboratory. Therefore the theoretical investigation is required to predict the relevant cross section data.     

44 利用ANC方法间接确定天体物理反应^26Si（p，γ）^27P的反应率

^26Al衰变放出能量为1．809MeV的γ射线，该射线在诸如新星、X射线爆炸等天体物理事件中是一个极好的观测量。^26Al主要通过反应链^24Mg（p，γ）^25Al（β^＋）^26Mg（p，γ）^26Al合成，然而^26Al的合成由于其短寿命（T1/2=6．34s）同质异能态的存在而变得复杂。^26Si（p，γ）^27P能跨越^26Al的主要产生链，是其合成过程中的重要反应之一。     

Indirect Measurement of Cross Section of ^9Be（p,α）^6Li

The cross section of ^9Be（p,α）^6Li at low energies is important for nuclear astrophysics. But it is difficult for direct measurement because of the Coulomb barrier and electron screening effect. In order to measure the 9Be（p,α）6Li bare nucleus cross section at astrophysical energies, the Trojan Horse Method（THM） can be applied. The main feature of the method is that it allows to extract the energy dependence for the bare astrophysical S（E） factor at very low energies without any extrapolation, by measuring the cross section of an appropriate three body process.