The $\mathrm{^2H}(d,p)\mathrm{^3H}$ bare nucleus astrophysical S(E) factor has been measured indirectly at energies from about 500 keV down to several keV by means of the Trojan-horse method applied to the quasi-free process $\mathrm{^2H({}^6Li},pt)\mathrm{^4He}$ induced at the lithium beam energy of 11 and 9.5 MeV, which makes the virtual binary process incident energy $\mathrm {E}_{dd}^{qf}$ go much closer to the zero-quasi-free-energy point than that in the previous similar experiment. The obtained results are compared with direct data as well as with previous indirect investigation of the same binary reactions. It shows that the precision of S(E) data in low energy range extracted via the same Trojan horse nucleus ($\mathrm{^6Li}=(d \oplus α)$ ) becomes better when the incident energy decreases from high value down to the zero-quasi-free-energy point. The very good agreement between data extracted from different Trojan horse nucleus ($\mathrm{^6Li}=(d \oplus α)$ vs. $\mathrm{^3He}=(d \oplus p)$) gives a strong updated test for the independence of the binary indirect cross section on the chosen Trojan horse nucleus at low energies.
Indirect Measurement of the $\rm S^*(E)$ Factor for $\rm {}^{12}C({}^{12}C,\mathit{p}){}^{23}Na$ at Gamow Energies via the Trojan Horse Method with Near-0 degree Spectator Detection
Institute of Radiation Technology, Beijing Academy of Science and Technology（北京应用技术研究院辐射技术研究所）
Big Bang Nucleosynthesis results refined via the Trojan Horse Method
Laboratori Nazionali del Sud, INFN（南方国家实验室，意大利核物理研究所）；Dipartimento di Fisica e Astronomia ‘Ettore Majorana’, Universitá di Catania（卡塔尼亚大学埃托雷·马约拉纳物理与天文学系）；Centro Siciliano di Fisica Nucleare e Struttura della Materia (CSFNSM)（西西里核物理与物质结构中心）；Sezione di Napoli, INFN（意大利核物理研究所那不勒斯分部）；Dipartimento di Fisica e Astronomia ’Galileo Galilei’,Universitá degli Studi di Padova（帕多瓦大学伽利略·伽利莱物理与天文学系）；Sezione di Padova, INFN（意大利核物理研究所帕多瓦分部）
$\rm S^*(E)$ measurement of the $\rm {}^{12}C({}^{12}C,α){}^{20}Ne$ reaction at astrophysical energies via the Trojan horse method with $\rm ^{16}O$ quasi-free breakup
Institute of Radiation Technology, Beijing Academy of Science and Technology（北京辐射技术研究所，北京 Akademija 科学技术研究院）；Department of Nuclear Physics, China Institute of Atomic Energy（原子能科学研究院核物理系）；School of Physics and Materials Science, Anhui University（安徽大学物理与材料科学学院）
Concurrent application of ANC and THM to assess the $^{13}{\rm C}(α,n)^{16}{\rm O}$ absolute cross section at astrophysical energies and possible consequences for neutron production in low-mass AGB stars
Multi-Model Analysis of the Astrophysical $S(E)$ Factor for the $^{9}\mathrm{Be}(p,α)^{6}\mathrm{Li}$ Reaction and Its Impact on Astrophysical Reaction Rates
School of Physics, Anhui University（安徽大学物理学院）；School of Physics, Southern University of Science and Technology（南方科技大学物理学院）；College of Physics and Optoelectronic Engineering, Shenzhen University（深圳大学物理与光电工程学院）；Institute of Radiation Technology, Beijing Academy of Science and Technology（北京市科学技术研究院辐射技术研究所）；Department of Nuclear Physics, China Institute of Atomic Energy（中国原子能科学研究院核物理系）
