Astrophysical SE2 factor of the C12(α,γ)O16 reaction through the C12(B11,Li7)O16 transfer reaction
| العنوان: | Astrophysical SE2 factor of the C12(α,γ)O16 reaction through the C12(B11,Li7)O16 transfer reaction |
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| المؤلفون: | Y. P. Shen, Q. W. Fan, S. Zeng, J. Su, Er-Tao Li, S. Q. Yan, Y. B. Wang, C. J. Pei, Z. D. An, J. C. Liu, Z. H. Li, Dan-Yang Pang, S. Adhikari, D. H. Li, T. L. Ma, B. Guo, L. Gan, Y. Zhou, Z. Y. Han, Y. J. Li, Y. Su, X. C. Du, W. P. Liu, X. Y. Li, G. Lian |
| المصدر: | Physical Review C. 99 |
| بيانات النشر: | American Physical Society (APS), 2019. |
| سنة النشر: | 2019 |
| مصطلحات موضوعية: | Physics, Transfer (group theory), Angular distribution, Resonance, Atomic physics, Tandem accelerator, Born approximation |
| الوصف: | The $^{12}\mathrm{C}(\ensuremath{\alpha},\ensuremath{\gamma})^{16}\mathrm{O}$ reaction plays a key role in the evolution of stars with masses of $Mg0.55\phantom{\rule{0.16em}{0ex}}{M}_{\ensuremath{\bigodot}}$. The cross-section of the $^{12}\mathrm{C}(\ensuremath{\alpha},\ensuremath{\gamma})^{16}\mathrm{O}$ reaction within the Gamow window (${E}_{\text{c.m.}}=300\phantom{\rule{0.16em}{0ex}}\mathrm{keV}, {T}_{9}=0.2$) is extremely small (about ${10}^{\ensuremath{-}17}$ barn), which makes the direct measurement in a ground-based laboratory with existing techniques unfeasible. Up until now, the cross-sections at lower energies can only be extrapolated from the data at higher energies. However, two subthreshold resonances, located at ${E}_{x}=7.117\phantom{\rule{0.16em}{0ex}}\mathrm{MeV}$ and ${E}_{x}=6.917\phantom{\rule{0.16em}{0ex}}\mathrm{MeV}$, make this extrapolation more complicated. In this work, the 6.917 MeV subthreshold resonance in the $^{12}\mathrm{C}(\ensuremath{\alpha},\ensuremath{\gamma})^{16}\mathrm{O}$ reaction was investigated via the $^{12}\mathrm{C}(^{11}\mathrm{B},^{7}\mathrm{Li})^{16}\mathrm{O}$ reaction. The experiment was performed using the Q3D magnetic spectrograph at the HI-13 tandem accelerator. We measured the angular distribution of the $^{12}\mathrm{C}(^{11}\mathrm{B},^{7}\mathrm{Li})^{16}\mathrm{O}$ transfer reaction leading to the 6.917 MeV state. Based on the finite-range distorted wave Born approximation (FRDWBA) and coupled-reaction-channel (CRC) analysis, we derived the asymptotic normalization coefficient (ANC) of the 6.917 MeV level in $^{16}\mathrm{O}$ to be ($1.10\ifmmode\pm\else\textpm\fi{}0.29$) $\ifmmode\times\else\texttimes\fi{}{10}^{10}\phantom{\rule{0.16em}{0ex}}{\mathrm{fm}}^{\ensuremath{-}1}$, with which the reduced $\ensuremath{\alpha}$ width was computed to be $18.0\ifmmode\pm\else\textpm\fi{}4.7\phantom{\rule{0.16em}{0ex}}\mathrm{keV}$ at the channel radius of 6.5 fm. Finally, we calculated the astrophysical ${S}_{E2}(300)$ factor of the ground-state transitions to be 46.2 $\ifmmode\pm\else\textpm\fi{}$ 7.7 keV b. The result for the astrophysical ${S}_{E2}(300)$ factor confirms the values obtained in various direct and indirect measurements and presents an independent examination of the most important data in nuclear astrophysics. |
| تدمد: | 2469-9993 2469-9985 |
| URL الوصول: | https://explore.openaire.eu/search/publication?articleId=doi_________::d29e6501d5690a42b2234894424b358b https://doi.org/10.1103/physrevc.99.025805 |
| حقوق: | OPEN |
| رقم الأكسشن: | edsair.doi...........d29e6501d5690a42b2234894424b358b |
| قاعدة البيانات: | OpenAIRE |
| تدمد: | 24699993 24699985 |
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