Study of neutron source reaction 13C(α, n)16O in stars

Bing Guo; Zhi Hong Li; M. Lugaro; J. Buntain; Dan Yang Pang; Yun Ju Li; Jun Su; Sheng Quan Yan; Zhi Dan Wu; Xi Xiang Bai; Yong Shou Chen; Xian Chao Du; Qi Wen Fan; Lin Gan; Sun Jun Jin; A. I. Karakas; Er Tao Li; Zhi Chang Li; Gang Lian; Jian Cheng Liu; Xin Liu; Jian Rong Shi; Neng Chuan Shu; Bao Xiang Wang; You Bao Wang; Sheng Zeng; Wei Ping Liu

doi:10.7538/yzk.2014.48.02.0193

Study of neutron source reaction ¹³C(α, n)¹⁶O in stars

Bing Guo^*, Zhi Hong Li, M. Lugaro, J. Buntain, Dan Yang Pang, Yun Ju Li, Jun Su, Sheng Quan Yan, Zhi Dan Wu, Xi Xiang Bai, Yong Shou Chen, Xian Chao Du, Qi Wen Fan, Lin Gan, Sun Jun Jin, A. I. Karakas, Er Tao Li, Zhi Chang Li, Gang Lian, Jian Cheng LiuXin Liu, Jian Rong Shi, Neng Chuan Shu, Bao Xiang Wang, You Bao Wang, Sheng Zeng, Wei Ping Liu

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

Abstract

¹³C(α,n)¹⁶O is the main neutron source reaction of slow neutron capture (s) process in asymptotic giant branch (AGB) stars. The 6.356 MeV 1/2⁺ subthreshold resonance in ¹⁷O plays an important role in the ¹³C(α,n)¹⁶O reaction. The ¹³C(¹¹B, ⁷Li)¹⁷O angular distributions were measured using HI-13 tandem accelerator and Q3D magnetic spectrograph, and then used to determine the α-width of the subthreshold resonant state which is currently the most uncertain parameter for determining the ¹³C(α,n)¹⁶O reaction rate. By using the present α-width, the astrophysical S-factor and the stellar rate of the ¹³C(α,n)¹⁶O reaction were derived. This shed some light on the existing discrepancies up to a factor of 25 in S-factors derived from different authors. The simulation of s-process in AGB stars shows that the new reaction rate produces 25% more Pb than the CF88 compilation.

Original language	English
Pages (from-to)	193-200
Number of pages	8
Journal	Yuanzineng Kexue Jishu/Atomic Energy Science and Technology
Volume	48
Issue number	2
DOIs	https://doi.org/10.7538/yzk.2014.48.02.0193
Publication status	Published - Feb 2014

Access to Document

10.7538/yzk.2014.48.02.0193

Cite this

Guo, B., Li, Z. H., Lugaro, M., Buntain, J., Pang, D. Y., Li, Y. J., Su, J., Yan, S. Q., Wu, Z. D., Bai, X. X., Chen, Y. S., Du, X. C., Fan, Q. W., Gan, L., Jin, S. J., Karakas, A. I., Li, E. T., Li, Z. C., Lian, G., ... Liu, W. P. (2014). Study of neutron source reaction ¹³C(α, n)¹⁶O in stars. Yuanzineng Kexue Jishu/Atomic Energy Science and Technology, 48(2), 193-200. https://doi.org/10.7538/yzk.2014.48.02.0193

@article{6c27977d84e141c4a36e415644f4a831,

title = "Study of neutron source reaction 13C(α, n)16O in stars",

abstract = "13C(α,n)16O is the main neutron source reaction of slow neutron capture (s) process in asymptotic giant branch (AGB) stars. The 6.356 MeV 1/2+ subthreshold resonance in 17O plays an important role in the 13C(α,n)16O reaction. The 13C(11B, 7Li)17O angular distributions were measured using HI-13 tandem accelerator and Q3D magnetic spectrograph, and then used to determine the α-width of the subthreshold resonant state which is currently the most uncertain parameter for determining the 13C(α,n)16O reaction rate. By using the present α-width, the astrophysical S-factor and the stellar rate of the 13C(α,n)16O reaction were derived. This shed some light on the existing discrepancies up to a factor of 25 in S-factors derived from different authors. The simulation of s-process in AGB stars shows that the new reaction rate produces 25% more Pb than the CF88 compilation.",

keywords = "AGB stars, Angular distribution of transfer reaction, Astrophysical S-factor, Subthreshold resonance, s-process",

author = "Bing Guo and Li, {Zhi Hong} and M. Lugaro and J. Buntain and Pang, {Dan Yang} and Li, {Yun Ju} and Jun Su and Yan, {Sheng Quan} and Wu, {Zhi Dan} and Bai, {Xi Xiang} and Chen, {Yong Shou} and Du, {Xian Chao} and Fan, {Qi Wen} and Lin Gan and Jin, {Sun Jun} and Karakas, {A. I.} and Li, {Er Tao} and Li, {Zhi Chang} and Gang Lian and Liu, {Jian Cheng} and Xin Liu and Shi, {Jian Rong} and Shu, {Neng Chuan} and Wang, {Bao Xiang} and Wang, {You Bao} and Sheng Zeng and Liu, {Wei Ping}",

year = "2014",

month = feb,

doi = "10.7538/yzk.2014.48.02.0193",

language = "English",

volume = "48",

pages = "193--200",

journal = "Yuanzineng Kexue Jishu/Atomic Energy Science and Technology",

issn = "1000-6931",

publisher = "Atomic Energy Publishing House",

number = "2",

}

Guo, B, Li, ZH, Lugaro, M, Buntain, J, Pang, DY, Li, YJ, Su, J, Yan, SQ, Wu, ZD, Bai, XX, Chen, YS, Du, XC, Fan, QW, Gan, L, Jin, SJ, Karakas, AI, Li, ET, Li, ZC, Lian, G, Liu, JC, Liu, X, Shi, JR, Shu, NC, Wang, BX, Wang, YB, Zeng, S & Liu, WP 2014, 'Study of neutron source reaction ¹³C(α, n)¹⁶O in stars', Yuanzineng Kexue Jishu/Atomic Energy Science and Technology, vol. 48, no. 2, pp. 193-200. https://doi.org/10.7538/yzk.2014.48.02.0193

TY - JOUR

T1 - Study of neutron source reaction 13C(α, n)16O in stars

AU - Guo, Bing

AU - Li, Zhi Hong

AU - Lugaro, M.

AU - Buntain, J.

AU - Pang, Dan Yang

AU - Li, Yun Ju

AU - Su, Jun

AU - Yan, Sheng Quan

AU - Wu, Zhi Dan

AU - Bai, Xi Xiang

AU - Chen, Yong Shou

AU - Du, Xian Chao

AU - Fan, Qi Wen

AU - Gan, Lin

AU - Jin, Sun Jun

AU - Karakas, A. I.

AU - Li, Er Tao

AU - Li, Zhi Chang

AU - Lian, Gang

AU - Liu, Jian Cheng

AU - Liu, Xin

AU - Shi, Jian Rong

AU - Shu, Neng Chuan

AU - Wang, Bao Xiang

AU - Wang, You Bao

AU - Zeng, Sheng

AU - Liu, Wei Ping

PY - 2014/2

Y1 - 2014/2

N2 - 13C(α,n)16O is the main neutron source reaction of slow neutron capture (s) process in asymptotic giant branch (AGB) stars. The 6.356 MeV 1/2+ subthreshold resonance in 17O plays an important role in the 13C(α,n)16O reaction. The 13C(11B, 7Li)17O angular distributions were measured using HI-13 tandem accelerator and Q3D magnetic spectrograph, and then used to determine the α-width of the subthreshold resonant state which is currently the most uncertain parameter for determining the 13C(α,n)16O reaction rate. By using the present α-width, the astrophysical S-factor and the stellar rate of the 13C(α,n)16O reaction were derived. This shed some light on the existing discrepancies up to a factor of 25 in S-factors derived from different authors. The simulation of s-process in AGB stars shows that the new reaction rate produces 25% more Pb than the CF88 compilation.

AB - 13C(α,n)16O is the main neutron source reaction of slow neutron capture (s) process in asymptotic giant branch (AGB) stars. The 6.356 MeV 1/2+ subthreshold resonance in 17O plays an important role in the 13C(α,n)16O reaction. The 13C(11B, 7Li)17O angular distributions were measured using HI-13 tandem accelerator and Q3D magnetic spectrograph, and then used to determine the α-width of the subthreshold resonant state which is currently the most uncertain parameter for determining the 13C(α,n)16O reaction rate. By using the present α-width, the astrophysical S-factor and the stellar rate of the 13C(α,n)16O reaction were derived. This shed some light on the existing discrepancies up to a factor of 25 in S-factors derived from different authors. The simulation of s-process in AGB stars shows that the new reaction rate produces 25% more Pb than the CF88 compilation.

KW - AGB stars

KW - Angular distribution of transfer reaction

KW - Astrophysical S-factor

KW - Subthreshold resonance

KW - s-process

UR - http://www.scopus.com/inward/record.url?scp=84896283837&partnerID=8YFLogxK

U2 - 10.7538/yzk.2014.48.02.0193

DO - 10.7538/yzk.2014.48.02.0193

M3 - Article

SN - 1000-6931

VL - 48

SP - 193

EP - 200

JO - Yuanzineng Kexue Jishu/Atomic Energy Science and Technology

JF - Yuanzineng Kexue Jishu/Atomic Energy Science and Technology

IS - 2

ER -

Study of neutron source reaction ¹³C(α, n)¹⁶O in stars

Abstract

Access to Document

Other files and links

Fingerprint

Cite this