Destruction of [Formula Presented] via [Formula Presented] burning through the [Formula Presented] keV resonance

D. W. Bardayan, ORNL Physics Division
J. C. Blackmon, ORNL Physics Division
W. Bradfield-Smith, Yale University
C. R. Brune, The University of North Carolina at Chapel Hill
A. E. Champagne, The University of North Carolina at Chapel Hill
T. Davinson, The University of Edinburgh
B. A. Johnson, Tennessee Technological University
R. L. Kozub, Tennessee Technological University
C. S. Lee, Chung-Ang University
R. Lewis, Yale University
P. D. Parker, Yale University
A. C. Shotter, The University of Edinburgh
M. S. Smith, ORNL Physics Division
D. W. Visser, Yale University
P. J. Woods, The University of Edinburgh


Knowledge of the astrophysical rate of the [Formula Presented] reaction is important for understanding the γ-ray emission expected from novae and heavy-element production in x-ray bursts. The rate of this reaction is dominated at temperatures above [Formula Presented] GK by a resonance near 7.08 MeV excitation energy in [Formula Presented] The [Formula Presented] rate has been uncertain in part because of disagreements among previous measurements concerning the resonance strength and excitation energy of this state. To resolve these uncertainties, we have made simultaneous measurements of the [Formula Presented] and [Formula Presented] excitation functions using a radioactive [Formula Presented] beam at the ORNL Holifield Radioactive Ion Beam Facility. A simultaneous fit of the data sets has been performed, and the best fit was obtained with a center-of-mass resonance energy of [Formula Presented] keV [Formula Presented] keV), a total width of [Formula Presented] keV, a proton branching ratio of [Formula Presented] and a resonance strength of [Formula Presented] keV. © 2001 The American Physical Society.