1986
DOI: 10.1016/0375-9474(86)90073-4
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Threshold states in 26Al revisited

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Cited by 31 publications
(21 citation statements)
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“…Unfortunately, some of the conclusions that they drew from their data were in error. Motivated by the 25 Mg(p,␥␥) studies of Endt et al (1986), improved, higher-resolution ( 3 He,d) measurements were performed (Champagne et al, 1986a) that produced a more reliable set of spectroscopic factors and reaction rates. A notable outcome of this work was the identification of a strong s-wave resonance at an energy of E c.m.…”
Section: Reaction Ratesmentioning
confidence: 99%
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“…Unfortunately, some of the conclusions that they drew from their data were in error. Motivated by the 25 Mg(p,␥␥) studies of Endt et al (1986), improved, higher-resolution ( 3 He,d) measurements were performed (Champagne et al, 1986a) that produced a more reliable set of spectroscopic factors and reaction rates. A notable outcome of this work was the identification of a strong s-wave resonance at an energy of E c.m.…”
Section: Reaction Ratesmentioning
confidence: 99%
“…However, Endt and Rolfs (1987) calculated reaction rates that were in disagreement with these results, primarily because of their use of square-well single-particle widths, but also because they overestimated several important spectroscopic factors. The situation was clarified by Champagne et al (1989) and Rollefson et al (1990) who produced rates consistent with one another and with Champagne et al (1986a) while also extending their analyses to include weakly populated states. Finally, Iliadis et al (1996) derived reaction rates from the existing data by employing a realistic diffuse optical model potential in the calculation of single particle widths.…”
Section: Reaction Ratesmentioning
confidence: 99%
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“…In fact, a f0 of about 80% was deduced in Champagne et al (1983a) and Champagne et al (1983b). However, the same authors quote a lower value of 61% in Champagne et al (1986). Finally, the compilation by Endt & Rolfs (1987) gives 85%.…”
Section: Final Remarksmentioning
confidence: 96%
“…The temperature range of astrophysical interests is T = 0.02-2 GK, so the levels between 50 keV and 310 keV are more important in the study of galactic 26 Al. Many experiments have been performed to study the 25 Mg(p, γ) 26 Al reaction sine 1970 [13][14][15][16][17][18][19][20][21][22][23][24], but the experiment on the surface of earth ground can only reach to 190 keV energy level due to the small cross section and large background effects of the cosmic rays. In 2012, the laboratory of underground nuclear astrophysics (LUNA) in Italy successfully measured the resonance strength at 92 keV with the help of high shielding conditions in the underground laboratory [25,26].…”
Section: Al Reactionmentioning
confidence: 99%