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First Direct Measurement of the 17F(p,gamma)18Ne Cross Section.

K A Chipps¹, D W Bardayan, J C Blackmon

¹Colorado School of Mines, Golden, Colorado 80401, USA.

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|June 13, 2009

Summary

Researchers directly measured the fluorine-17 (F-17) proton capture reaction, crucial for astrophysics. They determined the resonance strength of a key state in neon-18 (Ne-18), providing vital data for stellar models.

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Area of Science:

Nuclear astrophysics
Stellar nucleosynthesis
Radioactive ion beam physics

Background:

The (17)F(p,gamma)(18)Ne reaction rate is critical for understanding nucleosynthesis in stars.
A previously identified 3{+} state in (18)Ne significantly contributes to this reaction, but its strength was unquantified.

Purpose of the Study:

To directly measure the (17)F(p,gamma)(18)Ne reaction.
To determine the resonance strength of the 3{+} state in (18)Ne.
To constrain direct capture contributions to the reaction.

Main Methods:

Utilized a mixed beam of Fluorine-17 ((17)F) and Oxygen-17 ((17)O) at Oak Ridge National Laboratory (ORNL).
Performed direct measurements of the (17)F(p,gamma)(18)Ne reaction.

Main Results:

The resonance strength for the 3{+} resonance in (18)Ne was determined to be omegagamma = 33 +/- 14(stat) +/- 17(syst) meV.
This corresponds to a gamma width of Gamma_{gamma} = 56 +/- 24(stat) +/- 30(syst) meV.
An upper limit for direct capture was established at S(E) <= 65 keV b at 800 keV.

Conclusions:

The quantified resonance strength provides crucial data for astrophysical reaction network calculations.
The results refine our understanding of nucleosynthesis processes influenced by the (17)F(p,gamma)(18)Ne reaction.
The study establishes important constraints for stellar evolution models.