Synopsis: Nuclear star gazing

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Measurements of 31S energy levels and reevaluation of the thermonuclear resonant 30P(p,γ)31S reaction rate

C. Wrede, J. A. Caggiano, J. A. Clark, C. M. Deibel, A. Parikh, and P. D. Parker

Published April 10, 2009

Calculating thermonuclear reaction rates in stars requires detailed information about the cross sections for the relevant reactions. However, the nuclei involved in these reactions are often unstable and thus difficult to produce as a beam or target. While many researchers are actively pursuing new facilities to produce such radioactive beams, in some cases important nuclear physics information can be determined indirectly. In a paper appearing in Physical Review C, Christopher Wrede, now at the University of Washington, and collaborators at Yale University and TRIUMF in Vancouver, Canada, determine the reaction rate for proton capture by 30P that leads to 31S and a photon [the reaction is represented symbolically by 30P(p,γ)31S ]. They do this by measuring the detailed level structure in 31S using reactions with stable nuclear targets, even though 30P itself is unstable.

The 30P(p,γ)31S reaction is crucial to understanding nucleosynthesis in certain explosive environments such as novae, Type I x-ray bursts, and Type II supernovae. The authors use reactions involving stable 31P and 32S targets—in particular the 31P(3He,t)31S, 31P(3He,t)31S*(p)30P, and 32S(d,t)31S reactions—to extract resonance energies, spins, and proton branching ratios, which yield new information on the 30P(p,γ)31S reaction in the temperature range between ten million and ten billion degrees. They compare the measurements to nuclear statistical model calculations. Generally, statistical models are not useful for studying lighter nuclear systems where the level density is low, but the good agreement with Wrede et al.’s results suggest that the nuclear statistical model can be used for some lighter systems. – Brad Filippone

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