Properties of<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msup><mml:mrow><mml:mi mathvariant="normal">P</mml:mi></mml:mrow><mml:mrow><mml:mn>30</mml:mn></mml:mrow></mml:msup></mml:mrow></mml:math>Levels from the Reaction<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msup><mml:mrow><mml:mi mathvariant="normal">Si</mml:mi></mml:mrow><mml:mrow><mml:mn>29</mml:mn></mml:mrow></mml:msup></mml:mrow><mml:mo>(</mml:mo><mml:mi>p</m

Harris, Gale I.; Hyder, A. K.; Walinga, Jennifer

doi:10.1103/physrev.187.1413

Cited by 52 publications

(9 citation statements)

References 31 publications

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“…We find that our newly calculated strength for the 2 − , 315-keV resonance (ωγ ∼ 25 meV) is approximately twice as large as the most recent direct measurement [17], but agrees well with the value reported in Ref. [18]. As such, the 315-keV state is now expected to dominate the 29 Si(p, γ) 30 P reaction over the entire peak temperature range of ONe novae (T = 0.1 − 0.4 GK), and the overall rate is higher than previously reported [11], as shown in Fig.…”

supporting

confidence: 92%

“…In this regard, a key uncertainty relates to the unknown spinparity assignments of the 217-and 315-keV resonances. For instance, a spin assignment of J = 2 for the 315-keV resonance would support the strength reported by Harris et al [18] and not that of the most recent study [17]. In this paper, we employ a 28 Si( 3 He, p) fusion-evaporation reaction to perform an in-beam γ-ray spectroscopy study of the astrophysically important nucleus 30 P. The choice of a light-ion transfer reaction allows for a selective population of key low-spin proton-unbound resonant states, and for unambiguous determinations of spin-parity assignments.…”

supporting

confidence: 77%

“…All the hydrodynamic simulations performed in this work resulted in the ejection of ∼ 5 × 10 −6 M of nuclear-processed material, after achieving a peak temperature of ∼ 3.1 × 10 8 K. Nucleosynthesis results using the present 29 Si(p, γ) 30 P rate, a statistical model rate [23], as well as a high rate, based on the upper limit for the strength of the 315-keV resonance of Ref. [18], are displayed in Table II.…”

mentioning

confidence: 89%

“…The 402-keV resonance has been studied precisely using direct techniques [16]. However, very little information ex- ists on the 217-keV resonance and current direct measurements of the strength of the 315-keV state, in normal kinematics, differ by a factor ∼2 [17,18]. In this regard, a key uncertainty relates to the unknown spinparity assignments of the 217-and 315-keV resonances.…”

mentioning

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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supporting

confidence: 92%

supporting

confidence: 77%

mentioning

confidence: 89%

mentioning

confidence: 99%

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Spectroscopy of P30 and the abundance of Si29 in presolar grains

et al. 2020

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“…Harris and James (15) found that crops differed in their magnitude of response in changes of fatty acids with temperatures. Knowles (16) recently reviewed the safflower research in California in which varietal'differences in response of oil composition to temperature during seed maturation was established.…”

Section: Resultsmentioning

confidence: 99%

Effect of controlled temperature environments on oil content and on fatty acid composition of corn oil

Thompson

Jellum

Young

1973

J Americ Oil Chem Soc

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Total oil content and fatty acid composition of germ and endosperm oil were determined on grain from three inbred lines and one variety of corn (Zea mays L.) grown in four phytotron environments and one standard greenhouse environment during seed maturation. Pronounced differences occurred with reversals for relative percentages of oleic and linoleic acids of germ oil for one inbred line and for the variety. Comparative trends were generally less pronounced for two of the inbred lines. Differences among environments were less evident for palmitic, stearic, and linolenic acids of germ oil and for the fatty acids of the endosperm oil. Total oil was lowest for two inbred lines and the variety grown in the high temperature environment (30 C day/26 C night). The magnitude of temperature effects on oil content and oil composition varied among the four corn genotypes.

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15-Phosphorus

Sukhoruchkin

Soroko

2004

Tables of Proton and Α-Particle Resonance Parameters. Part 1

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Properties ofP30Levels from the ReactionSi29(p

Cited by 52 publications

References 31 publications

Spectroscopy of P30 and the abundance of Si29 in presolar grains

Spectroscopy of P30 and the abundance of Si29 in presolar grains

Effect of controlled temperature environments on oil content and on fatty acid composition of corn oil

15-Phosphorus

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