The 59Fe (n,γ) 60Fe Cross Section from the Surrogate Ratio Method and Its Effect on the 60Fe Nucleosynthesis

doi:10.3847/1538-4357/ac12ce

	The 59Fe (n,γ) 60Fe Cross Section from the Surrogate Ratio Method and Its Effect on the 60Fe Nucleosynthesis
	Yan,S. Q.1; Li,X. Y.1; Nishio,K.2; Lugaro,M.3,4,5; Li,Z. H.1,8; Makii,H.2; Pignatari,M.3,11,12; Wang,Y. B.1; Orlandi,R.2; Hirose,K.2
刊名	The Astrophysical Journal
	2021-09-28
卷号	919 期号:2
关键词	Nuclear physics Stellar nucleosynthesis Massive stars
ISSN号	0004-637X
DOI	10.3847/1538-4357/ac12ce
通讯作者	Yan,S. Q.()
英文摘要	Abstract The long-lived 60Fe (with a half-life of 2.62 Myr) is a crucial diagnostic of active nucleosynthesis in the Milky Way galaxy and in supernovae near the solar system. The neutron-capture reaction 59Fe(n,γ)60Fe on 59Fe (half-life = 44.5 days) is the key reaction for the production of 60Fe in massive stars. This reaction cross section has been previously constrained by the Coulomb dissociation experiment, which offered partial constraint on the E1 γ-ray strength function but a negligible constraint on the M1 and E2 components. In this work, for the first time, we use the surrogate ratio method to experimentally determine the 59Fe(n,γ)60Fe cross sections in which all the components are included. We derived a Maxwellian-averaged cross section of 27.5 ± 3.5 mb at kT = 30 keV and 13.4 ± 1.7 mb at kT = 90 keV, roughly 10%–20% higher than previous estimates. We analyzed the impact of our new reaction rates in nucleosynthesis models of massive stars and found that uncertainties in the production of 60Fe from the 59Fe(n,γ)60Fe rate are at most 25%. We conclude that stellar physics uncertainties now play a major role in the accurate evaluation of the stellar production of 60Fe.
语种	英语
出版者	The American Astronomical Society
WOS记录号	IOP:0004-637X-919-2-AC12CE
内容类型	期刊论文
源URL	[http://119.78.100.186/handle/113462/136556]
专题	中国科学院近代物理研究所
通讯作者	Yan,S. Q.
作者单位	1.China Institute of Atomic Energy, P. O. Box 275(10), Beijing 102413, People’s Republic of China; panyu@ciae.ac.cn; wpliu@ciae.ac.cn 2.Japan Atomic Energy Agency, Tokai, Ibaraki 319-1195, Japan 3.Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, E?tv?s Loránd Research Network (ELKH), Konkoly Thege Miklós út 15-17, 1121 Budapest, Hungary; maria.lugaro@csfk.org 4.ELTE E?tv?s Loránd University, Institute of Physics, Budapest 1117, Pázmány Péter sétány 1/A, Hungary 5.School of Physics and Astronomy, Monash University, VIC 3800, Australia 6.Institute for Nuclear Research (ATOMKI), H-4001 Debrecen, Hungary 7.Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou 730000, People’s Republic of China 8.School of Nuclear Science and Technology, University of Chinese Academy of Sciences, Beijing, 100080, People’s Republic of China 9.School of Nuclear Science and Technology, Lanzhou University, Lanzhou 730000, People’s Republic of China 10.Beijing Normal University, Beijing 100875, People’s Republic of China
推荐引用方式 GB/T 7714	Yan,S. Q.,Li,X. Y.,Nishio,K.,et al. The 59Fe (n,γ) 60Fe Cross Section from the Surrogate Ratio Method and Its Effect on the 60Fe Nucleosynthesis[J]. The Astrophysical Journal,2021,919(2).
APA	Yan,S. Q..,Li,X. Y..,Nishio,K..,Lugaro,M..,Li,Z. H..,...&Liu,W. P..(2021).The 59Fe (n,γ) 60Fe Cross Section from the Surrogate Ratio Method and Its Effect on the 60Fe Nucleosynthesis.The Astrophysical Journal,919(2).
MLA	Yan,S. Q.,et al."The 59Fe (n,γ) 60Fe Cross Section from the Surrogate Ratio Method and Its Effect on the 60Fe Nucleosynthesis".The Astrophysical Journal 919.2(2021).