期刊
PHYSICAL REVIEW C
卷 101, 期 4, 页码 -出版社
AMER PHYSICAL SOC
DOI: 10.1103/PhysRevC.101.045802
关键词
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资金
- National Science Foundation [Phys-1713857]
- Joint Institute for Nuclear Astrophysics [Phys-0822648, PHY-1430152]
- U.S. D.O.E. [DE-FG02-88ER40387, DE-NA0003883]
- U.S. Department of Energy [DE-AC52-07NA27344]
The C-13(alpha, n)O-16 reaction is the main source of neutrons for the s and i processes in asymptotic giant branch stars and carbon-enhanced metal-poor stars, respectively. The reaction rate over the relevant temperature range from 0.1 to 0.3 GK translates into a center-of-mass energy range of 150 to 540 keV. Current measurements extend down to 300 keV, still requiring an extrapolation of the cross section. At these low energies, the high-energy tail of a 1/2(+) state near the reaction threshold makes a significant contribution to the cross section, but its amplitude is still highly uncertain. In this paper the uncertainties associated with the low-energy cross-section extrapolation are investigated, in particular the sensitivity to the energy, width, and Coulomb renormalized asymptotic normalization coefficient of the near-threshold resonance. Recently it has been suggested that the energy of the near-threshold level may have a large impact on the extrapolation, but this is not found to be the case compared with the other sources of uncertainty.
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