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S. Parete-Koon, W. Hix (U. Tennessee), M. Smith (ORNL Physics Division), S. Starrfield (Arizona State U.), D. Bardayan (U. North Carolina; ORNL Physics Division), M. Guidry (U. Tennessee; ORNL Physics Division), A. Mezzacappa (ORNL Physics Division)
Proton capture by 17F plays an important role in nova explosions. A revised rate for this reaction has been determined based on measurements of the 1H (17F,p)17F excitation function using a radioactive 17F beam at ORNL's Holifield Radioactive Ion Beam Facility. We have used this new rate in calculations of the nucleosynthesis resulting from nova outbursts on the surfaces of 1.25 M and 1.35 M solar mass ONeMg white dwarfs (WD) and a 1.00 solar mass CO WD. We find that the new reaction rate changes the abundances of some nuclides (e.g. 17O) synthesized in the innermost regions of the explosion on the 1.35 solar mass WD by more than a factor of 10,000 compared to some previous estimates, and by more than factor of 3 when the entire exploding envelope is considered. The calculations for the 1.25 solar mass WD nova show that this new rate changes the abundances of some nuclides synthesized in the innermost regions by more than a factor of 600 compared to some previous estimates, and by more than a factor of 2 when the entire exploding envelope is considered. Calculations for the 1.00 solar mass WD nova show that this new rate changes the abundance of 18Ne by 20.6 all other nuclides. A comparison of model predictions with observation will also be discussed.
ORNL Physics Divisioni is Managed by UT-Battelle, LLC, for the U.S. Department of Energy under contract DE-AC05-00OR22725.
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Bulletin of the American Astronomical Society, 34, #4
© 2002. The American Astronomical Soceity.