Measurement of the sulfur-32(p,d)sulfur-31 reaction and its astrophysical implications

Details Measurement of the sulfur-32(p,d)sulfur-31 reaction and its astrophysical implications Measurement of the sulfur-32(p,d)sulfur-31 reaction and its astrophysical implications

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006phdt........37m&link_type=abstract

Proquest Dissertations And Theses 2006. Section 0226, Part 0606 132 pages; [Ph.D. dissertation].United States -- Tennessee: The

Computer Science

4

Sulfur, Cross Sections, Phosphorus, Excitation Energies

Scientific paper

The 30 P(p,[gamma]) 31 S reaction plays a crucial role in the synthesis of heavier nuclear species, from Si to Ca, in nova outbursts on ONe White Dwarfs [26, 28, 35]. However, its rate is very uncertain as a result of the lack of spectroscopic information on the levels above proton threshold in 31 S. The currently adopted rate of this reaction, based on statistical Hauser-Feshbach calculations [36], could have an uncertainty as much as a factor of 100 higher or lower under nova conditions [26].
To reduce these uncertainties, we have measured differential cross sections for the 32 S(p,d) 31 S reaction and determined excitation energies for states in 31 S. A total of 26 states in 31 S were observed, including 17 above the proton threshold. Five new states were observed. Uncertainties in the excitation energies of states in the high energy region were significantly reduced. Spin and parity values were determined or constrained for 15 of the strongly populated levels through a distorted wave Born approximation (DWBA) analysis of the angular distributions, of which 6 were made for the first time.
A new 30 P(p,[gamma]) 31 S reaction rate was calculated utilizing the present experimental spectroscopic information. We confirmed the spin-parity assignment of 1/2 + for the state at 6263 keV which dominates the 30 P(p,[gamma]) 31 S reaction rate at lower temperatures in nova, while the state at 6544 keV dominates at temperatures above 0.2 GK (1 GK=1.0×10 9 Kelvin). Our results indicate that the 30 P(p,[gamma]) 31 S rate based on our resonance calculations is reduced by up to a factor of 10 at nova temperatures compared to the previous rate.
Nova element synthesis calculations using the new 30 P(p,[gamma]) 31 S reaction rate were performed, and predictions of isotopic abundance patterns were obtained. Production of elements in the Si-Ca mass region are found to be altered by as much as 40% using the new rate. Important isotopic ratios are found to agree well with observations on presolar grains thought to have a nova origin [34]. Of special interest are the close-to-solar 29 Si/ 28 Si ratio and large excess in 30 Si/ 28 Si found in our simulations, which are the most important features pointing to a nova origin of such grains.

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