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84 results on '"Bai, X. X."'

1. Electronic Structures of Black Phosphorus Studied by Angle-resolved Photoemission Spectroscopy

Author

Han, C. Q., Yao, M. Y., Bai, X. X., Miao, Lin, Zhu, Fengfeng, Guan, D. D., Wang, Shun, Gao, C. L., Liu, Canhua, Qian, Dong, Liu, Y., and Jia, Jin-feng

Subjects
Condensed Matter - Materials Science
Abstract

Electronic structures of single crystalline black phosphorus were studied by state-of-art angleresolved photoemission spectroscopy. Through high resolution photon energy dependence measurements, the band dispersions along out-of-plane and in-plane directions are experimentally determined. The electrons were found to be more localized in the ab-plane than that is predicted in calculations. Beside the kz-dispersive bulk bands, resonant surface state is also observed in the momentum space. Our finds strongly suggest that more details need to be considered to fully understand the electronic properties of black phosphorus theoretically.

Published
2014
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2. Proton widths of the low-lying 16F states from the 15N(7Li, 6Li)16N reaction

Author

Wu, Z. D., Guo, B., Li, Z. H., Li, Y. J., Su, J., Pang, D. Y., Yan, S. Q., Li, E. T., Bai, X. X., Du, X. C., Fan, Q. W., Gan, L., He, J. J., Jin, S. J., Jing, L., Li, L., Li, Z. C., Lian, G., Liu, J. C., Shen, Y. P., Wang, Y. B., Yu, X. Q., Zeng, S., Zhang, D. H., Zhang, L. Y., Zhang, W. J., and Liu, W. P.

Subjects
Nuclear Experiment
Abstract

All the 16F levels are unbound by proton emission. To date the four low-lying 16F levels below 1 MeV have been experimentally identified with well established spin-parity values and excitation energies with an accuracy of 4 - 6 keV. However, there are still considerable discrepancies for their level widths. The present work aims to explore these level widths through an independent method. The angular distributions of the 15N(7Li, 6Li)16N reaction leading to the first four states in 16N were measured using a high-precision Q3D magnetic spectrograph. The neutron spectroscopic factors and the asymptotic normalization coefficients for these states in 16N were then derived based on distorted wave Born approximation analysis. The proton widths of the four low-lying resonant states in 16F were obtained according to charge symmetry of strong interaction., Comment: 14 pages, 6 figures, 4 tables

Published
2014
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3. Spectroscopic factors for low-lying 16N levels and the astrophysical 15N(n,gamma)16N reaction rate

Author

Guo, B., Li, Z. H., Li, Y. J., Su, J., Pang, D. Y., Yan, S. Q., Wu, Z. D., Li, E. T., Bai, X. X., Du, X. C., Fan, Q. W., Gan, L., He, J. J., Jin, S. J., Jing, L., Li, L., Li, Z. C., Lian, G., Liu, J. C., Shen, Y. P., Wang, Y. B., Yu, X. Q., Zeng, S., Zhang, L. Y., Zhang, W. J., and Liu, W. P.

Subjects
Nuclear Experiment
Abstract

Fluorine is a key element for nucleosynthetic studies since it is extremely sensitive to the physical conditions within stars. The astrophysical site to produce fluorine is suggested to be asymptotic giant branch (AGB) stars. In these stars the 15N(n, g)16N reaction could affect the abundance of fluorine by competing with 15N(a, g)19F. The 15N(n, g)16N reaction rate depends directly on the neutron spectroscopic factors of the low-lying states in 16N. The angular distributions of the 15N(7Li, 6Li)16N reaction populating the ground state and the first three excited states in 16N are measured using a Q3D magnetic spectrograph and are used to derive the spectroscopic factors of these states based on distorted wave Born approximation (DWBA) analysis. The spectroscopic factors of these four states are extracted to be 0.96+-0.09, 0.69+-0.09, 0.84+-0.08 and 0.65+-0.08, respectively. Based on the new spectroscopic factors we derive the 15N(n,g)16N reaction rate. The accuracy and precision of the spectroscopic factors are enhanced due to the first application of high-precision magnetic spectrograph for resolving the closely-spaced 16N levels which can not be achieved in most recent measurement. The present result demonstrates that two levels corresponding to neutron transfers to the 2s1/2 orbit in 16N are not so good single-particle levels although 15N is a closed neutron-shell nucleus. This finding is contrary to the shell model expectation. The present work also provides an independent examination to shed some light on the existing discrepancies in the spectroscopic factors and the 15N(n, g)16N rate., Comment: 13 pages, 4 figures, 2 tables

Published
2013
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4. Determination of astrophysical 12N(p,g)13O reaction rate from the 2H(12N, 13O)n reaction and its astrophysical implications

Author

Guo, B., Su, J., Li, Zhihong, Wang, Y. B., Yan, S. Q., Li, Y. J., Shu, N. C., Han, Y. L., Bai, X. X., Chen, Y. S., Liu, W. P., Yamaguchi, H., Binh, D. N., Hashimoto, T., Hayakawa, S., Kahl, D., Kubono, S., He, J. J., Hu, J., Xu, S. W., Iwasa, N., Kume, N., and Li, Zhihuan

Subjects
Nuclear Experiment
Abstract

The evolution of massive stars with very low-metallicities depends critically on the amount of CNO nuclides which they produce. The $^{12}$N($p$,\,$\gamma$)$^{13}$O reaction is an important branching point in the rap-processes, which are believed to be alternative paths to the slow 3$\alpha$ process for producing CNO seed nuclei and thus could change the fate of massive stars. In the present work, the angular distribution of the $^2$H($^{12}$N,\,$^{13}$O)$n$ proton transfer reaction at $E_{\mathrm{c.m.}}$ = 8.4 MeV has been measured for the first time. Based on the Johnson-Soper approach, the square of the asymptotic normalization coefficient (ANC) for the virtual decay of $^{13}$O$_\mathrm{g.s.}$ $\rightarrow$ $^{12}$N + $p$ was extracted to be 3.92 $\pm$ 1.47 fm$^{-1}$ from the measured angular distribution and utilized to compute the direct component in the $^{12}$N($p$,\,$\gamma$)$^{13}$O reaction. The direct astrophysical S-factor at zero energy was then found to be 0.39 $\pm$ 0.15 keV b. By considering the direct capture into the ground state of $^{13}$O, the resonant capture via the first excited state of $^{13}$O and their interference, we determined the total astrophysical S-factors and rates of the $^{12}$N($p$,\,$\gamma$)$^{13}$O reaction. The new rate is two orders of magnitude slower than that from the REACLIB compilation. Our reaction network calculations with the present rate imply that $^{12}$N($p,\,\gamma$)$^{13}$O will only compete successfully with the $\beta^+$ decay of $^{12}$N at higher ($\sim$two orders of magnitude) densities than initially predicted., Comment: 8 figures, 2 tables, Submitted to Physical Review C

Published
2012
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5. New determination of the 13C(a, n)16O reaction rate and its influence on the s-process nucleosynthesis in AGB stars

Author

Guo, B., Li, Z. H., Lugaro, M., Buntain, J., Pang, D. Y., Li, Y. J., Su, J., Yan, S. Q., Bai, X. X., Chen, Y. S., Fan, Q. W., Jin, S. J., Karakas, A. I., Li, E. T., Li, Z. C., Lian, G., Liu, J. C., Liu, X., Shi, J. R., Shu, N. C., Wang, B. X., Wang, Y. B., Zeng, S., and Liu, W. P.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Nuclear Experiment
Abstract

We present a new measurement of the $\alpha$-spectroscopic factor ($S_\alpha$) and the asymptotic normalization coefficient (ANC) for the 6.356 MeV 1/2$^+$ subthreshold state of $^{17}$O through the $^{13}$C($^{11}$B, $^{7}$Li)$^{17}$O transfer reaction and we determine the $\alpha$-width of this state. This is believed to have a strong effect on the rate of the $^{13}$C($\alpha$, $n$)$^{16}$O reaction, the main neutron source for {\it slow} neutron captures (the $s$-process) in asymptotic giant branch (AGB) stars. Based on the new width we derive the astrophysical S-factor and the stellar rate of the $^{13}$C($\alpha$, $n$)$^{16}$O reaction. At a temperature of 100 MK our rate is roughly two times larger than that by \citet{cau88} and two times smaller than that recommended by the NACRE compilation. We use the new rate and different rates available in the literature as input in simulations of AGB stars to study their influence on the abundances of selected $s$-process elements and isotopic ratios. There are no changes in the final results using the different rates for the $^{13}$C($\alpha$, $n$)$^{16}$O reaction when the $^{13}$C burns completely in radiative conditions. When the $^{13}$C burns in convective conditions, as in stars of initial mass lower than $\sim$2 $M_\sun$ and in post-AGB stars, some changes are to be expected, e.g., of up to 25% for Pb in our models. These variations will have to be carefully analyzed when more accurate stellar mixing models and more precise observational constraints are available.

Published
2012
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6. Asymptotic normalization coefficient from the 12C(7Li,6He)13N reaction and the astrophysical 12C(p,g)13N reaction rate

Author

Li, Z. H., Su, J., Guo, B., Li, Z. C., Bai, X. X., Liu, J. C., Li, Y. J., Yan, S. Q., Wang, B. X., Wang, Y. B., Lian, G., Zeng, S., Li, E. T., Fang, X., Liu, W. P., Chen, Y. S., Shu, N. C., and Fan, Q. W.

Subjects
Nuclear Experiment
Abstract

Angular distribution of the 12C(7Li,6He)13N reaction at E(7Li) = 44.0 MeV was measured at the HI-13 tandem accelerator of Beijing, China. Asymptotic normalization coefficient (ANC) of 13N = 12C + p was derived to be 1.64 $\pm$ 0.11 fm$^{-1/2}$ through distorted wave Born approximation (DWBA) analysis. The ANC was then used to deduce the astrophysical $S(E)$ factors and reaction rates for direct capture in 12C(p,g)13N at energies of astrophysical relevance., Comment: 13 pages, 4 figues, submitted to Nucl. Phys. A

Published
2009

7. Composition analysis of 1,495 cases of upper urinary tract calculi: the role of age and gender.

Author

TU, X., ZHUANG, X.-Y., BAI, X.-X., and HUANG, C.-Y.

Abstract

OBJECTIVE: This study aimed to quantitatively analyze the calculi components of upper urinary tract calculi and to explore the relationship between calculus components, demographic characteristics, and underlying diseases. PATIENTS AND METHODS: Clinical data of 1,495 patients with upper urinary tract calculi were retrospectively collected. The calculi were divided into simple calcium oxalate, calcium oxalate mixed, calcium phosphate mixed, uric acid, magnesium ammonium phosphate, and other components. Statistical software SPSS 22.0 was used to analyze the differences between the stone compositions and various factors. The influencing factors (p < 0.05) were analyzed using multiple logistic regression analysis. RESULTS: Among 1,495 patients with upper urinary tract calculi, simple calcium oxalate calculi were the most common component (39.7%), followed by calcium oxalate mixed calculi (30.4%), uric acid calculi (13.6%), calcium phosphate mixed calculi (10.4%), magnesium ammonium phosphate calculi (5.8%) and other component calculi (0.1%). Univariate analysis revealed statistically significant differences in stone composition according to gender, age, and hyperuricemia (p < 0.05). Multiple logistic regression analysis showed that compared to men, the odds ratio (OR) values of calcium oxalate mixed stones, calcium phosphate mixed stones, and magnesium ammonium phosphate stones in women were 1.61, 2.50, and 4.17, respectively (p < 0.001). Compared with elderly patients, the OR values of calcium phosphate mixed stones in young and middle-aged patients were 3.14 and 2.70, respectively (p < 0.05). CONCLUSIONS: Patients with different stone components had different demographic characteristics, and stone components were significantly different between gender and age. Calcium oxalate mixed stones were more common in females, and calcium phosphate mixed stones and magnesium ammonium phosphate stones were more common in females, young patients, and middle-aged patients. [ABSTRACT FROM AUTHOR]

Published
2024

11. Optical potential parameters from 12C + Zr elastic scattering

Author

Gan L., Li Z. H., Sun H. B., Su J., Li Y. J., Yan S. Q., Wang Y. B., Zeng S., Bai X. X., Du X. C., Wu Z. D., Jin S. J., Zhang W. J., Liu W. P., and Li E. T.

Subjects
Physics, QC1-999
Abstract

The angular distributions of 12C + 90,92,94,96Zr elastic scattering were measured with the Q3D magnetic spectrometer at the HI-13 tandem accelerator, Beijing. The real part of optical potential were extracted by analysing these angular distributions. The analysis enable us to avoid the influence of Coulomb effect and to observe the dependence of optical potential on the nuclear properties. With the deduced potential parameters, the experimental elastic scattering angular distributions can be reproduced very well. Formulas to infer global heavy-ion potential parameters were obtained then by analyzing the extracted optical potential parameters. The formulas can be used widely in heavy-ion nuclear reactions.

Published
2016
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12. Indirect measurement of the 57.7 keV resonance strength for the astrophysical γ -ray source of the Mg25(p,γ)Al26 reaction

Author

Li, Y. J., primary, Li, Z. H., additional, Li, E. T., additional, Li, X. Y., additional, Ma, T. L., additional, Shen, Y. P., additional, Liu, J. C., additional, Gan, L., additional, Su, Y., additional, Qiao, L. H., additional, Han, Z. Y., additional, Zhou, Y., additional, Su, J., additional, Yan, S. Q., additional, Zeng, S., additional, Wang, Y. B., additional, Guo, B., additional, Lian, G., additional, Nan, D., additional, Bai, X. X., additional, and Liu, W. P., additional

Published
2020
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15. Spectroscopic factors for low-lying 16N levels and the astrophysical 15N(n,gamma)16N reaction rate

Author

Guo, B., Li, Z. H., Li, Y. J., Su, J., Pang, D. Y., Yan, S. Q., Wu, Z. D., Li, E. T., Bai, X. X., Du, X. C., Fan, Q. W., Gan, L., He, J. J., Jin, S. J., Jing, L., Li, L., Li, Z. C., Lian, G., Liu, J. C., Shen, Y. P., Wang, Y. B., Yu, X. Q., Zeng, S., Zhang, L. Y., Zhang, W. J., and Liu, W. P.

Subjects
FOS: Physical sciences, Nuclear Experiment (nucl-ex), Nuclear Experiment
Abstract

Fluorine is a key element for nucleosynthetic studies since it is extremely sensitive to the physical conditions within stars. The astrophysical site to produce fluorine is suggested to be asymptotic giant branch (AGB) stars. In these stars the 15N(n, g)16N reaction could affect the abundance of fluorine by competing with 15N(a, g)19F. The 15N(n, g)16N reaction rate depends directly on the neutron spectroscopic factors of the low-lying states in 16N. The angular distributions of the 15N(7Li, 6Li)16N reaction populating the ground state and the first three excited states in 16N are measured using a Q3D magnetic spectrograph and are used to derive the spectroscopic factors of these states based on distorted wave Born approximation (DWBA) analysis. The spectroscopic factors of these four states are extracted to be 0.96+-0.09, 0.69+-0.09, 0.84+-0.08 and 0.65+-0.08, respectively. Based on the new spectroscopic factors we derive the 15N(n,g)16N reaction rate. The accuracy and precision of the spectroscopic factors are enhanced due to the first application of high-precision magnetic spectrograph for resolving the closely-spaced 16N levels which can not be achieved in most recent measurement. The present result demonstrates that two levels corresponding to neutron transfers to the 2s1/2 orbit in 16N are not so good single-particle levels although 15N is a closed neutron-shell nucleus. This finding is contrary to the shell model expectation. The present work also provides an independent examination to shed some light on the existing discrepancies in the spectroscopic factors and the 15N(n, g)16N rate., Comment: 13 pages, 4 figures, 2 tables

Published
2014
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16. Radii of the bound states in 16 N from the asymptotic normalization coefficients

Author

Li, E. T., primary, Guo, B., additional, Li, Z. H., additional, Wang, Y. B., additional, Li, Y. J., additional, Wu, Z. D., additional, Su, J., additional, Pang, D. Y., additional, Bai, X. X., additional, Du, X. C., additional, Fan, Q. W., additional, Gan, L., additional, Han, Z. Y., additional, Hao, X., additional, Hu, S. P., additional, He, J. J., additional, Jing, L., additional, Jin, S. J., additional, Li, L., additional, Li, X. Y., additional, Li, Z. C., additional, Lian, G., additional, Liu, J. C., additional, Luo, Q., additional, Qiao, L. H., additional, Shen, Y. P., additional, Sun, H. B., additional, Yan, S. Q., additional, Yu, X. Q., additional, Zeng, S., additional, Zhang, D. H., additional, Zhang, L. Y., additional, Zhang, W. J., additional, Zhou, Y., additional, and Liu, W. P., additional

Published
2016
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17. Examination of the surrogate ratio method for the determination of theZr93(n,γ)Zr94cross section withZr90,92(O18,O16)Zr92,94reactions

Author

Yan, S. Q., primary, Li, Z. H., additional, Wang, Y. B., additional, Nishio, K., additional, Makii, H., additional, Su, J., additional, Li, Y. J., additional, Nishinaka, I., additional, Hirose, K., additional, Han, Y. L., additional, Orlandi, R., additional, Shen, Y. P., additional, Guo, B., additional, Zeng, S., additional, Lian, G., additional, Chen, Y. S., additional, Bai, X. X., additional, Qiao, L. H., additional, and Liu, W. P., additional

Published
2016
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19. Optical potential parameters from12C + Zr elastic scattering

Author

Gan, L., primary, Li, Z. H., additional, Sun, H. B., additional, Su, J., additional, Li, Y. J., additional, Yan, S. Q., additional, Wang, Y. B., additional, Zeng, S., additional, Bai, X. X., additional, Du, X. C., additional, Wu, Z. D., additional, Jin, S. J., additional, Zhang, W. J., additional, Liu, W. P., additional, and Li, E. T., additional

Published
2016
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20. Measurement of theFe52mass via the precise proton-decay energy ofCom53

Author

Shen, Y. P., primary, Liu, W. P., additional, Su, J., additional, Zhang, N. T., additional, Jing, L., additional, Li, Z. H., additional, Wang, Y. B., additional, Guo, B., additional, Yan, S. Q., additional, Li, Y. J., additional, Zeng, S., additional, Lian, G., additional, Du, X. C., additional, Gan, L., additional, Bai, X. X., additional, Wang, J. S., additional, Zhang, Y. H., additional, Zhou, X. H., additional, Tang, X. D., additional, He, J. J., additional, Yang, Y. Y., additional, Jin, S. L., additional, Ma, P., additional, Ma, J. B., additional, Huang, M. R., additional, Bai, Z., additional, Zhou, Y. J., additional, Ma, W. H., additional, Hu, J., additional, Xu, S. W., additional, Ma, S. B., additional, Chen, S. Z., additional, Zhang, L. Y., additional, and Ding, B., additional

Published
2015
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21. Proton spectroscopic factor of the12Cground state from the12C(11B,12C)11Belastic transfer reaction

Author

Li, E. T., primary, Li, Z. H., additional, Li, Y. J., additional, Guo, B., additional, Wang, Y. B., additional, Pang, D. Y., additional, Su, J., additional, Yan, S. Q., additional, Zeng, S., additional, Gan, L., additional, Li, Z. C., additional, Liu, J. C., additional, Bai, X. X., additional, Wu, Z. D., additional, Jin, S. J., additional, Zhang, L. Y., additional, Yu, X. Q., additional, Li, L., additional, Sun, H. B., additional, Lian, G., additional, Fan, Q. W., additional, and Liu, W. P., additional

Published
2014
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22. Optical potential parameters from 12C + Zr elastic scattering.

Author

Gan, L., Li, Z. H., Sun, H. B., Su, J., Li, Y. J., Yan, S. Q., Wang, Y. B., Zeng, S., Bai, X. X., Du, X. C., Wu, Z. D., Jin, S. J., Zhang, W. J., Liu, W. P., and Li, E. T.

Subjects
ELASTIC scattering, MAGNETIC spectrometer, TANDEM accelerators, ANGULAR distribution (Nuclear physics), HEAVY ion collisions
Abstract

The angular distributions of 12C + 90,92,94,96zr elastic scattering were measured with the Q3D magnetic spectrometer at the HI-13 tandem accelerator, Beijing. The real part of optical potential were extracted by analysing these angular distributions. The analysis enable us to avoid the influence of Coulomb effect and to observe the dependence of optical potential on the nuclear properties. With the deduced potential parameters, the experimental elastic scattering angular distributions can be reproduced very well. Formulas to infer global heavy-ion potential parameters were obtained then by analyzing the extracted optical potential parameters. The formulas can be used widely in heavy-ion nuclear reactions. [ABSTRACT FROM AUTHOR]

Published
2016
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23. Two measurements of the 22Na+p resonant scattering via thicktarget inverse-kinematics method.

Author

Wang, Y. B., Jin, S. J., Jing, L., Han, Z. Y., Bai, X. X., Guo, B., Li, Y. J., Li, Z. H., Lian, G., Su, J., Sun, L. J., Yan, S. Q., Zeng, S., Liu, W. P., Yamaguchi, H., Kubono, S., Hu, J., Kahl, D., He, J. J., and Wang, J. S.

Subjects
ELASTIC scattering, SODIUM, KINEMATICS, RADIOISOTOPES, RADIOACTIVITY, CHARGE exchange reactions, EXCITATION energy (In situ microanalysis)
Abstract

22Na is an important isotope for the study of extinct radioactivity, meanwhile its sufficiently long half life provides the possibility to observe live 22Na in nearby nova explosions. The 22Na(p,γ)23Mg is one of the key reactions that influence the 22Na abundance in nova ejecta. To study the proton resonant states in 23Mg relevant to the astrophysical 22Na(p,γ)23Mg reaction rates, two measurements have been carried out at the CRIB separator of University of Tokyo, and the RIBLL secondary beamline in Lanzhou, respectively. The 22Na secondary beam was produced via the ¹H(22Ne, 22Na)n charge exchange reaction. Thick-target inverse-kinematics method is applied to obtain the excitation function of 22Na+p elastic scattering. Extended gas target and solid state polyethylene foil were used in the two measurements, respectively, to map the different excitation energy region of the compound nucleus 23Mg. Several new resonant levels are observed and their contribution to the 22Na(p,γ)23Mg reaction rate is evaluated. [ABSTRACT FROM AUTHOR]

Published
2016
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26. Proton widths of the low-lying16Fstates from the15N(7Li,6Li)16Nreaction

Author

Wu, Z. D., primary, Guo, B., additional, Li, Z. H., additional, Li, Y. J., additional, Su, J., additional, Pang, D. Y., additional, Yan, S. Q., additional, Li, E. T., additional, Bai, X. X., additional, Du, X. C., additional, Fan, Q. W., additional, Gan, L., additional, He, J. J., additional, Jin, S. J., additional, Jing, L., additional, Li, L., additional, Li, Z. C., additional, Lian, G., additional, Liu, J. C., additional, Shen, Y. P., additional, Wang, Y. B., additional, Yu, X. Q., additional, Zeng, S., additional, Zhang, D. H., additional, Zhang, L. Y., additional, Zhang, W. J., additional, and Liu, W. P., additional

Published
2014
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27. Spectroscopic factors for low-lyingN16levels and the astrophysicalN15(n,γ)N16reaction rate

Author

Guo, B., primary, Li, Z. H., additional, Li, Y. J., additional, Su, J., additional, Pang, D. Y., additional, Yan, S. Q., additional, Wu, Z. D., additional, Li, E. T., additional, Bai, X. X., additional, Du, X. C., additional, Fan, Q. W., additional, Gan, L., additional, He, J. J., additional, Jin, S. J., additional, Jing, L., additional, Li, L., additional, Li, Z. C., additional, Lian, G., additional, Liu, J. C., additional, Shen, Y. P., additional, Wang, Y. B., additional, Yu, X. Q., additional, Zeng, S., additional, Zhang, L. Y., additional, Zhang, W. J., additional, and Liu, W. P., additional

Published
2014
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28. Resonant scattering of22Na + pstudied by the thick-target inverse-kinematic method

Author

Jin, S. J., primary, Wang, Y. B., additional, Su, J., additional, Yan, S. Q., additional, Li, Y. J., additional, Guo, B., additional, Li, Z. H., additional, Zeng, S., additional, Lian, G., additional, Bai, X. X., additional, Liu, W. P., additional, Yamaguchi, H., additional, Kubono, S., additional, Hu, J., additional, Kahl, D., additional, Jung, H. S., additional, Moon, J. Y., additional, Lee, C. S., additional, Teranishi, T., additional, Wang, H. W., additional, Ishiyama, H., additional, Iwasa, N., additional, Komatsubara, T., additional, and Brown, B. A., additional

Published
2013
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29. Erratum to: New determination of the astrophysical 13 C( p, $ \gamma$ 14 N S(E) factors and reaction rates via the 13 C( 7 Li, 6 He) 14 N reaction

Author

Li, Y. J., primary, Li, Z. H., additional, Li, E. T., additional, Bai, X. X., additional, Su, J., additional, Guo, B., additional, Wang, B. X., additional, Yan, S. Q., additional, Zeng, S., additional, Li, Z. C., additional, Liu, J. C., additional, Liu, X., additional, Jin, S. J., additional, Wang, Y. B., additional, Zhang, L. Y., additional, Yu, X. Q., additional, Li, L., additional, Lian, G., additional, Fan, Q. W., additional, and Liu, W. P., additional

Published
2013
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30. Erratum: New determination of the proton spectroscopic factor in9Befrom the13C(9Be,8Li)14Nangular distribution [Phys. Rev. C87, 017601 (2013)]

Author

Li, Z. H., primary, Li, Y. J., additional, Su, J., additional, Guo, B., additional, Li, E. T., additional, Dong, K. J., additional, Bai, X. X., additional, Li, Z. C., additional, Liu, J. C., additional, Yan, S. Q., additional, Wang, Y. B., additional, Zeng, S., additional, Lian, G., additional, Wang, B. X., additional, Jin, S. J., additional, Liu, X., additional, Zhang, W. J., additional, Huang, W. Z., additional, Fan, Q. W., additional, Gan, L., additional, Wu, Z. D., additional, and Liu, W. P., additional

Published
2013
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31. Reexamining theβdecay of53,54Ni,52,53Co,51Fe, and50Mn

Author

Su, J., primary, Liu, W. P., additional, Shu, N. C., additional, Yan, S. Q., additional, Li, Z. H., additional, Guo, B., additional, Huang, W. Z., additional, Zeng, S., additional, Li, E. T., additional, Jin, S. J., additional, Liu, X., additional, Wang, Y. B., additional, Lian, G., additional, Li, Y. J., additional, Chen, Y. S., additional, Bai, X. X., additional, Wang, J. S., additional, Yang, Y. Y., additional, Chen, R. F., additional, Xu, S. W., additional, Hu, J., additional, Chen, S. Z., additional, Ma, S. B., additional, Han, J. L., additional, Ma, P., additional, Hu, Q., additional, Ma, J. B., additional, Cao, X. G., additional, Jin, S. L., additional, Bai, Z., additional, Yang, K., additional, Shi, F. D., additional, Zhang, W., additional, Chen, Z., additional, Liu, L. X., additional, Lin, Q. Y., additional, Yan, X. S., additional, Zhang, X. H., additional, Fu, F., additional, He, J. J., additional, Li, X. Q., additional, He, C., additional, and Smith, M. S., additional

Published
2013
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32. Determination of the astrophysical12N(p,γ)13O reaction rate from the2H(12N,13O)nreaction and its astrophysical implications

Author

Guo, B., primary, Su, J., additional, Li, Z. H., additional, Wang, Y. B., additional, Yan, S. Q., additional, Li, Y. J., additional, Shu, N. C., additional, Han, Y. L., additional, Bai, X. X., additional, Chen, Y. S., additional, Liu, W. P., additional, Yamaguchi, H., additional, Binh, D. N., additional, Hashimoto, T., additional, Hayakawa, S., additional, Kahl, D., additional, Kubono, S., additional, He, J. J., additional, Hu, J., additional, Xu, S. W., additional, Iwasa, N., additional, and Kume, N., additional

Published
2013
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33. New determination of the proton spectroscopic factor in9Be from the13C(9Be,8Li)14N angular distribution

Author

Li, Z. H., primary, Li, Y. J., additional, Su, J., additional, Guo, B., additional, Li, E. T., additional, Dong, K. J., additional, Bai, X. X., additional, Li, Z. C., additional, Liu, J. C., additional, Yan, S. Q., additional, Wang, Y. B., additional, Zeng, S., additional, Lian, G., additional, Wang, B. X., additional, Jin, S. J., additional, Liu, X., additional, Zhang, W. J., additional, Huang, W. Z., additional, Fan, Q. W., additional, Gan, L., additional, Wu, Z. D., additional, and Liu, W. P., additional

Published
2013
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34. The half-lives of [sup 50]Mn, [sup 51]Fe, [sup 52,53]Co, and [sup 53,54]Ni

Author

Su, J., primary, Liu, W. P., additional, Shu, N. C., additional, Yan, S. Q., additional, Smith, M. S., additional, Wang, J. S., additional, Yang, Y. Y., additional, Li, X. Q., additional, He, C., additional, Li, Z. H., additional, Guo, B., additional, Huang, W. Z., additional, Zeng, S., additional, Li, E. T., additional, Jin, S. J., additional, Liu, X., additional, Wang, Y. B., additional, Lian, G., additional, Li, Y. J., additional, Chen, Y. S., additional, and Bai, X. X., additional

Published
2013
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35. NEW DETERMINATION OF THE13C(α,n)16O REACTION RATE AND ITS INFLUENCE ON THEs-PROCESS NUCLEOSYNTHESIS IN AGB STARS

Author

Guo, B., primary, Li, Z. H., additional, Lugaro, M., additional, Buntain, J., additional, Pang, D. Y., additional, Li, Y. J., additional, Su, J., additional, Yan, S. Q., additional, Bai, X. X., additional, Chen, Y. S., additional, Fan, Q. W., additional, Jin, S. J., additional, Karakas, A. I., additional, Li, E. T., additional, Li, Z. C., additional, Lian, G., additional, Liu, J. C., additional, Liu, X., additional, Shi, J. R., additional, Shu, N. C., additional, Wang, B. X., additional, Wang, Y. B., additional, Zeng, S., additional, and Liu, W. P., additional

Published
2012
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36. Indirect measurements of reactions in hot p-p chain and CNO cycles

Author

Wang, Y. B., primary, Guo, B., additional, Jin, S. J., additional, Li, Z. H., additional, Binh, D. N., additional, Hashimoto, H., additional, Hayakawa, S., additional, He, J. J., additional, Hu, J., additional, Iwasa, N., additional, Kahl, D. M., additional, Kubono, S., additional, Kume, N., additional, Li, E. T., additional, Li, Y. J., additional, Liu, X., additional, Su, J., additional, Xu, S. W., additional, Yamaguchi, H., additional, Yan, S. Q., additional, Zeng, S., additional, Bai, X. X., additional, Lian, G., additional, Wang, B. X., additional, and Liu, W. P., additional

Published
2012
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39. Indirect measurement of nuclear reactions of astrophysical interest

Author

Liu, W. P., primary, Li, Z. H., additional, Bai, X. X., additional, Wang, Y. B., additional, Guo, B., additional, Lian, G., additional, Su, J., additional, Zeng, S., additional, Wang, B. X., additional, Yan, S. Q., additional, Li, Y. J., additional, Li, E. T., additional, Jin, S. J., additional, Ozawa, Akira, additional, and Lu, Weiping, additional

Published
2010
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40. N13+pelastic resonance scattering via a thick-target method

Author

Wang, Y. B., primary, Wang, B. X., additional, Qin, X., additional, Bai, X. X., additional, Guo, B., additional, Jiang, C., additional, Li, Y. J., additional, Li, Z. H., additional, Lian, G., additional, Su, J., additional, Zeng, S., additional, and Liu, W. P., additional

Published
2008
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42. N13(d,n)O14reaction and the astrophysicalN13(p,γ)O14reaction rate

Author

Li, Z. H., primary, Guo, B., additional, Yan, S. Q., additional, Lian, G., additional, Bai, X. X., additional, Wang, Y. B., additional, Zeng, S., additional, Su, J., additional, Wang, B. X., additional, Liu, W. P., additional, Shu, N. C., additional, Chen, Y. S., additional, Chang, H. W., additional, and Jiang, L. Y., additional

Published
2006
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46. TheLi8(d,p)Li9reaction and the astrophysicalLi8(n,γ)Li9reaction rate

Author

Li, Z. H., primary, Liu, W. P., additional, Bai, X. X., additional, Guo, B., additional, Lian, G., additional, Yan, S. Q., additional, Wang, B. X., additional, Zeng, S., additional, Lu, Y., additional, Su, J., additional, Chen, Y. S., additional, Wu, K. S., additional, Shu, N. C., additional, and Kajino, T., additional

Published
2005
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47. STUDY OF ELASTIC RESONANCE SCATTERING AT CIAE.

Author

WANG, Y. B., JIN, S. J., WANG, B. X., LIU, X., BAI, X. X., LI, Z. H., LIAN, G., GUO, B., ZENG, S., SU, J., YAN, S. Q., QIN, X., LI, Y. J., LI, E. T., and LIU, W. P.

Subjects
PARTICLE beams, X-ray diffraction, KINEMATICS, RESONANCE, ELECTRONIC excitation
Published
2011

48. Indirect measurement of nuclear reactions of astrophysical interest.

Author

Liu, W. P., Li, Z. H., Bai, X. X., Wang, Y. B., Guo, B., Lian, G., Su, J., Zeng, S., Wang, B. X., Yan, S. Q., Li, Y. J., Li, E. T., and Jin, S. J.

Subjects
NUCLEAR reactions, ANGULAR correlations (Nuclear physics), COLLISIONS (Nuclear physics), CHEMICAL kinetics, ION bombardment
Abstract

Systematic indirect measurements of nuclear astrophysical reactions using the unstable ion beam facility GIRAFFE in CIAE were performed. We have measured the angular distributions of transfer reactions, such as 8Li(d,p)9Li, 8Li(d,n)9Be and 8Li(p,d)7Li in inverse kinematics, and derived the astrophysical S-factors or reaction rates for 8Li(n,γ)9Li and 8Li(p,γ)9Be by using asymptotic normalization coefficient (ANC) or spectroscopic factor methods. [ABSTRACT FROM AUTHOR]

Published
2010
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50. Alpha decay half-life of Sm in metal samarium and SmO.

Author

Su, J., Li, Z. H., Zhu, L. C., Lian, G., Bai, X. X., Wang, Y. B., Guo, B., Wang, B. X., Yan, S. Q., Zeng, S., Li, Y. J., Li, E. T., Jin, S. J., Liu, X., Fan, Q. W., Zhang, J. L., Jiang, X. Y., Lu, J. X., Lan, X. F., and Tang, X. Z.

Subjects
SAMARIUM, ALPHA decay, METALS, RADIOACTIVE decay, RADIOISOTOPE decay
Abstract

In order to investigate the possible influence of metallic environment on the alpha decay process, we have measured the Sm activities in the hosts of metal samarium and SmO . The Sm half-life was found to be (1.06±0.01)×10 y in metal samarium and (1.07±0.01)×10 y in SmO , respectively. No significant change has been observed within the experimental uncertainty. The absolute half-life presented here is consistent with the recommended value. [ABSTRACT FROM AUTHOR]

Published
2010
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