The 14O(α,p)17F reaction rate
J. C. Blackmon, ORNL Physics Division
D. W. Bardayan, ORNL Physics Division
W. Bradfield-Smith, Yale University
R. Brummitt, Tennessee Technological University
A. E. Champagne, The University of North Carolina at Chapel Hill
A. A. Chen, Yale University
T. Davinson, The University of Edinburgh
L. Dessieux, The University of Tennessee, Knoxville
M. W. Guidry, The University of Tennessee, Knoxville
K. I. Hahn, Ewha Womans University
G. M. Hale, Los Alamos National Laboratory Theoretical Division
W. R. Hix, ORNL Physics Division
R. L. Kozub, Tennessee Technological University
Z. Ma, ORNL Physics Division
P. D. Parker, Yale University
G. Rajbaidya, ORNL Physics Division
R. C. Runkle, The University of North Carolina at Chapel Hill
C. M. Rowland, The University of North Carolina at Chapel Hill
A. C. Shotter, The University of Edinburgh
M. S. Smith, ORNL Physics Division
L. A. Van Wormer, Hiram College
D. W. Visser, Yale University
P. J. Woods, The University of Edinburgh
Abstract
The 14O(α,p)17F reaction is an important part of the hot CNO cycle. We have measured cross sections for the 17F(p,p)17Fgs, 17F(p,p1)17F*495, and 17F(p,α)14O reactions in inverse kinematics using radioactive 17F beams from the Holifield Radioactive Ion Beam Facility. The properties of states in 18Ne, including those important for the 14O(α,p 17F reaction rate, were determined from an R-matrix analysis of the measured cross sections. An improved 14O(α,p 17F reaction rate has been determined. The hot CNO cycle of reactions is important in explosive astrophysical environments such as novae and X-ray bursts. In this cycle, proton captures by 12C and 13N in succession lead to the production of 14O. Destruction of 14O occurs by 14O(β+)14N and by the 14O(α,p)17F reaction. The slow rate of this reaction can limit energy generation and result in substantial abundances of the 14O isotope in novae [1] and X-ray bursts [2].
