The scattering of alpha particles from 12C and the stellar reaction rate

Plaga, R.; Becker, H.W.; Redder, A.; Rolfs, C.; Trautvetter, H. P.; Langanke, K.

doi:10.1016/0375-9474(87)90436-2

Cited by 131 publications

(136 citation statements)

References 29 publications

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“…Their results for the E1 part of the cross section essentially confirmed their earlier extrapolated value S E1 (E 0 )ϭ(79Ϯ21) keV b, and for the E2 part, established the upper limit S E2 (E 0 )Ͻ 140 keV b. Hale (1996) recently reported an R-matrix analysis of the E1 cross section alone that also used the elasticscattering angular-distribution data of Plaga et al (1987) rather than the P wave scattering phase shift. This analysis indicated that a rather low value of S E1 (E 0 ), 20 keV b, was consistent with all the measured data, including those of the ␤-delayed ␣ spectrum.…”

Section: Other Analyses and Recommended Valuessupporting

confidence: 58%

“…The importance of the subthreshold 1 Ϫ state at EϭϪ45 keV (E x ϭ7.11685 MeV) in fitting and extrapolating the E1 cross section was first demonstrated by Dyer and Barnes (1974). Most subsequent analyses have fit S factors extracted from the measurements along with the P wave phase shift obtained from ␣ϩ 12 C elastic scattering measurements (Plaga et al, 1987), using either R-matrix or K-matrix theory. More recently, several groups have acted on the longstanding suggestion of Barker (1971) to measure the ␤-delayed ␣ spectrum from the decay of 16 N with the hope of better determining the contribution of the subthreshold state, which is evident in the spectrum as a secondary maximum at low energies.…”

Section: E1 Capturementioning

confidence: 99%

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Synthesis of the elements in stars: forty years of progress

et al. 1997

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Forty years ago Burbidge, Burbidge, Fowler, and Hoyle combined what we would now call fragmentary evidence from nuclear physics, stellar evolution and the abundances of elements and isotopes in the solar system as well as a few stars into a synthesis of remarkable ingenuity. Their review provided a foundation for forty years of research in all of the aspects of low energy nuclear experiments and theory, stellar modeling over a wide range of mass and composition, and abundance studies of many hundreds of stars, many of which have shown distinct evidence of the processes suggested by B 2 FH. In this review we summarize progress in each of these fields with emphasis on the most recent developments. [S0034-6861(97)

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Section: Other Analyses and Recommended Valuessupporting

confidence: 58%

Section: E1 Capturementioning

confidence: 99%

Synthesis of the elements in stars: forty years of progress

et al. 1997

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“…A good description of the excitation functions below E c.m. = 5 MeV [10,12] is also obtained (figure 2). The potential in the present study seems to be comparable to the folding potential with the M3Y interaction [7,11,13,14].…”

mentioning

confidence: 76%

α+¹²C rotational bands in¹⁶O

Katsuma

2014

EPJ Web of Conferences

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“…The capture cross section is given as σ αγ ∝ ⟨ϕ f |ẽM E λ |ϕ i ⟩ 2 , where M E λ is the electric operator of Eλ transition. To generate the scattering state ϕ i , I use the potential describing elastic scattering [3,6,7]. The α+ 12 C cluster structure in 16 O is semi-classically defined by the evaluation of refractive scattering [8,9].…”

Section: Potential Model and Resultsmentioning

confidence: 99%