Excited states of30P investigated through the29Si(3He,d)30P reaction

Hertzog, R.C.; Green, L L; Green, M W; Jones, G.D.

doi:10.1088/0305-4470/7/1/015

Cited by 10 publications

(4 citation statements)

References 16 publications

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“…For an evaluation of the astrophysical 29 Si(p, γ) 30 P reaction rate, we consider all resonances from E r = 0 − 500 keV and use the new, precise resonance energies, together with our unambiguous spin-parity assignments. Proton spectroscopic factors, C 2 S, for the determination of resonance strengths have been taken, where available, from earlier ( 3 He,d) reaction studies [15,20]. In particular values of 0.01 and 0.17 [15], have been adopted for the 217 and 500 keV resonances, respectively, while an average value of C 2 S = 0.17 [15,20] has been used for the 315-keV resonance.…”

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confidence: 99%

“…Proton spectroscopic factors, C 2 S, for the determination of resonance strengths have been taken, where available, from earlier ( 3 He,d) reaction studies [15,20]. In particular values of 0.01 and 0.17 [15], have been adopted for the 217 and 500 keV resonances, respectively, while an average value of C 2 S = 0.17 [15,20] has been used for the 315-keV resonance. All other resonances are assumed to have nominal spectroscopic factors of C 2 S = 0.01, except the 402-keV resonance, for which we adopt the direct resonance strength measurement reported in Ref.…”

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confidence: 99%

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Spectroscopy of P30 and the abundance of Si29 in presolar grains

et al. 2020

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The astrophysical 29 Si(p, γ) reaction is expected to play a key role in determining the final 29 Si yields ejected in nova explosions. Such yields are used to accurately identify the stellar origins of meteoritic stardust and recently, distinctive silicon isotopic ratios have been extracted from a number of presolar grains. Here, the light-ion 28 Si( 3 He,p) fusion-evaporation reaction was used to populate low-spin, proton-unbound excited states in the nucleus 30 P that govern the rate of the astrophysical 29 Si(p, γ) reaction. In particular, γ decays were observed from resonances up to Er = 500 keV and key resonances at 217 and 315 keV have now been identified as 2 + and 2 − levels, respectively. Present calculations indicate that the strength of the 315 keV resonance, which dominates the rate of the 29 Si(p, γ) reaction over the entire temperature range of Oxygen-Neon (ONe) novae, is considerably higher than previously expected and as such, significantly affects the abundance of 29 Si ejected during novae explosions. In contrast, the 217 keV resonance is expected to make a negligible contribution to the 29 Si(p, γ) reaction rate, even at relatively low temperatures (T ∼ 0.1 GK).

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confidence: 99%

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Spectroscopy of P30 and the abundance of Si29 in presolar grains

et al. 2020

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“…[11] used the average of the spectroscopic factor values reported in Refs. [33,54] and found, from Eq. ( 3), a strength of ≈ (2 + 1)Γ ∕4 = 0.025 eV.…”

Section: Comparison Of Results To Ref [11]mentioning

confidence: 99%

Thermonuclear reaction rate of $^{29}$Si(p,$γ$)$^{30}$P

Downen,

Iliadis,

Champagne

et al. 2022

Preprint

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The thermonuclear rate of the 29 Si(p, ) 30 P reaction impacts the 29 Si abundance in classical novae. A reliable reaction rate is essential for testing the nova paternity of presolar stardust grains. At present, the fact that no classical nova grains have been unambiguously identified in primitive meteorites among thousands of grains studied is puzzling, considering that classical novae are expected to be prolific producers of dust grains. We investigated the 29 Si + reaction at center-of-mass energies of 200 − 420 keV, and present improved values for resonance energies, level excitation energies, resonance strengths, and branching ratios. One new resonance was found at a center-of-mass energy of 303 keV. For an expected resonance at 215 keV, an experimental upper limit could be determined for the strength. We evaluated the level structure near the proton threshold, and present new reaction rates based on all the available experimental information. Our new reaction rates have much reduced uncertainties compared to previous results at temperatures of ≥ 140 MK, which are most important for classical nova nucleosynthesis. Future experiments to improve the reaction rates at lower temperatures are discussed.

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“…Our motivation and our aim is to demonstrate, that the use of an appropriate model allows for a dramatic error reduction. The error reduction in this domain is of a crucial importance, since there is an effort to decrease even more the experimental error [6] and so, if one wants to solve the g−2 puzzle, the theoretical precision will have to follow.…”

Section: Introductionmentioning

confidence: 99%