期刊
PHYSICAL REVIEW C
卷 95, 期 5, 页码 -出版社
AMER PHYSICAL SOC
DOI: 10.1103/PhysRevC.95.055803
关键词
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资金
- National Science Foundation [PHY-1068192]
- Joint Institute for Nuclear Astrophysics Center for the Evolution of the Elements [PHY-0822648, PHY-1430152]
- South African National Research Foundation
- US Department of Energy, Office of Science, Office of Nuclear Physics [DE-SC0009883]
- Direct For Mathematical & Physical Scien
- Division Of Physics [1430152] Funding Source: National Science Foundation
The Ar-34(alpha, p)K-37 reaction is believed to be one of the last in a sequence of (alpha, p) and (p, gamma) reactions within the T-z = -1, sd-shell nuclei, known as the alpha p-process. This process is expected to influence the shape and rise times of luminosity curves coming from type I x-ray bursts (XRBs). With very little experimental information known on many of the reactions within the alpha p-process, stellar rates are calculated using a statistical model, such as Hauser-Feshbach. Questions on the applicability of a Hauser-Feshbach model for the Ar-34(alpha, p)K-37 reaction arise due to level density considerations in the compound nucleus, Ca-38. We have performed high energy-resolution forward-angle Ca-40(p, t)Ca-38 measurements with the K = 600 spectrograph at iThemba LABS in order to identify levels above the alpha-threshold in Ca-38. States identified in this work were then used to determine the Ar-34(alpha, p)K-37 reaction rate based on a narrow-resonance formalism. Comparisons are made to two standard Hauser-Feshbach model predicted rates at XRB temperatures.
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