恒星中子源13C(α, n)16O反应的研究

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 Hong 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

恒星中子源¹³C(α, n)¹⁶O反应的研究

Translated title of the contribution: 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 Hong Li, Gang Lian, Jian Cheng LiuXin Liu, Jian Rong Shi, Neng Chuan Shu, Bao Xiang Wang, You Bao Wang, Sheng Zeng, Wei Ping Liu

School of Physics and Astronomy

Research output: Contribution to journal › Article › Research › 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.

Translated title of the contribution	Study of neutron source reaction ¹³C(α, n)¹⁶O in stars
Original language	Chinese
Pages (from-to)	193-200
Number of pages	8
Journal	Yuanzineng Kexue Jishu
Volume	48
Issue number	2
DOIs	https://doi.org/10.7538/yzk.2014.48.02.0193
Publication status	Published - 2014

Keywords

AGB stars
Angular distribution of transfer reaction
Astrophysical S-factor
s-process
Subthreshold resonance

Access to Document

10.7538/yzk.2014.48.02.0193

Cite this

@article{e1255010ccc1456ba9ae4a5e4fff8c69,

title = "恒星中子源13C(α, n)16O反应的研究",

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, s-process, Subthreshold resonance",

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 Qi-Wen Fan and Lin Gan and Jin, {Sun Jun} and Karakas, {A. I.} and Li, {Er Tao} and Li, {Zhi Hong} 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",

doi = "10.7538/yzk.2014.48.02.0193",

language = "Chinese",

volume = "48",

pages = "193--200",

journal = "Yuanzineng Kexue Jishu",

issn = "1000-6931",

publisher = "China Institute of Atomic Energy",

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, Q-W, Gan, L, Jin, SJ, Karakas, AI, Li, ET, Li, ZH, Lian, G, Liu, JC, Liu, X, Shi, JR, Shu, NC, Wang, BX, Wang, YB, Zeng, S & Liu, WP 2014, '恒星中子源¹³C(α, n)¹⁶O反应的研究', Yuanzineng Kexue Jishu, vol. 48, no. 2, pp. 193-200. https://doi.org/10.7538/yzk.2014.48.02.0193

TY - JOUR

T1 - 恒星中子源13C(α, n)16O反应的研究

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 Hong

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

Y1 - 2014

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 - s-process

KW - Subthreshold resonance

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

AN - SCOPUS:84896283837

VL - 48

SP - 193

EP - 200

JO - Yuanzineng Kexue Jishu

JF - Yuanzineng Kexue Jishu

SN - 1000-6931

IS - 2