Strength of the 18F(p, α)15O resonance at Ec.m. = 330 keV
D. W. Bardayan, ORNL Physics Division
J. C. Batchelder, Oak Ridge Associated Universities
J. C. Blackmon, ORNL Physics Division
A. E. Champagne, The University of North Carolina at Chapel Hill
T. Davinson, The University of Edinburgh
R. Fitzgerald, The University of North Carolina at Chapel Hill
W. R. Hix, ORNL Physics Division
C. Iliadis, The University of North Carolina at Chapel Hill
R. L. Kozub, Tennessee Technological University
Z. Ma, The University of Tennessee, Knoxville
S. Parete-Koon, ORNL Physics Division
P. D. Parker, Yale University
N. Shu, ORNL Physics Division
M. S. Smith, ORNL Physics Division
P. J. Woods, The University of Edinburgh
Abstract
The astrophysical rate of the 18F(p,α)15O reaction at nova temperatures is critical to understanding production of the radioisotope 18F, which may be used to constrain nova models via observations with the coming generation of satellite-based γ-ray telescopes. As such, a measurement is made of the strength of this resonance using a radioactive 18F beam at the HRIBF. As a result, it is indicated that the 18F(p,α)15O reaction rate is lower than previous estimates by a factor of ∼2.
