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

Yan, S. Q.; Li, X. Y.; Nishio, K.; Lugaro, M.; Li, Z. H.; Makii, H.; Pignatari, M.; Wang, Y. B.; Orlandi, R.; Hirose, K.; Tsukada, K.; Mohr, P.; Li, G. S.; Wang, J. G.; Gao, B. S.; Han, Y. L.; Guo, B.; Li, Y. J.; Shen, Y. P.; Sato, T. K.; Ito, Y.; Suzaki, F.; Su, J.; Yang, Y. Y.; Wang, J. S.; Ma, J. B.; Ma, P.; Bai, Z.; Xu, S. W.; Ren, J.; Fan, Q. W.; Zeng, S.; Han, Z. Y.; Nan, W.; Nan, W. K.; Chen, C.; Lian, G.; Hu, Q.; Duan, F. F.; Jin, S. Y.; Tang, X. D.; Liu, W. P.

Authors

S. Q. Yan

X. Y. Li

K. Nishio

M. Lugaro

Z. H. Li

H. Makii

M. Pignatari

Y. B. Wang

R. Orlandi

K. Hirose

K. Tsukada

P. Mohr

G. S. Li

J. G. Wang

B. S. Gao

Y. L. Han

B. Guo

Y. J. Li

Y. P. Shen

T. K. Sato

Y. Ito

F. Suzaki

J. Su

Y. Y. Yang

J. S. Wang

J. B. Ma

P. Ma

Z. Bai

S. W. Xu

J. Ren

Q. W. Fan

S. Zeng

Z. Y. Han

W. Nan

W. K. Nan

C. Chen

G. Lian

Q. Hu

F. F. Duan

S. Y. Jin

X. D. Tang

W. P. Liu



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.

Citation

Yan, S. Q., Li, X. Y., Nishio, K., Lugaro, M., Li, Z. H., Makii, 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), Article 84. https://doi.org/10.3847/1538-4357/ac12ce

Journal Article Type Article
Acceptance Date Jul 8, 2021
Online Publication Date Sep 28, 2021
Publication Date Oct 1, 2021
Deposit Date Nov 19, 2021
Publicly Available Date Mar 29, 2024
Journal Astrophysical Journal
Print ISSN 0004-637X
Electronic ISSN 1538-4357
Publisher American Astronomical Society
Peer Reviewed Peer Reviewed
Volume 919
Issue 2
Article Number 84
DOI https://doi.org/10.3847/1538-4357/ac12ce
Keywords Nuclear physics; Stellar nucleosynthesis; Massive stars
Public URL https://hull-repository.worktribe.com/output/3858749

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Copyright Statement
This is an author-created, un-copyedited version of an article accepted for publication in The Astrophysical Journal. The publisher is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The Version of Record is available online at https://doi.org/10.3847/1538-4357/ac12ce





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