Cross sections for the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi mathvariant="normal">Li</mml:mi></mml:mrow><mml:mprescripts /><mml:mrow /><mml:mrow><mml:mn>6</mml:mn></mml:mrow><mml:mrow /><mml:mrow /></mml:mmultiscripts></mml:mrow></mml:math>(<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>p</mml:mi></mml:math>,<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow>

Elwyn, A.J.; Holland, Robert E.; Davids, C. N.; Meyer-Schützmeister, L.; Mooring, F.P.; Ray, William J.

doi:10.1103/physrevc.20.1984

Cited by 45 publications

(19 citation statements)

References 21 publications

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“…In Fig. 7 we compare the results for the S-factor with both 6 Li and 3 He cluster polarization with the available experimental cross section data [62][63][64][65][66][67][68][69][70]. Notations and data are taken from [71] and the web site http://pntpm.ulb.ac.be.…”

Section: The Reaction 6 Li(p 3 He) 4 Hementioning

confidence: 96%

A microscopic three-cluster model with nuclear polarization applied to the resonances of 7Be and the reaction 6Li(p, 3He)4He

et al. 2009

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A microscopic model for three-cluster configurations in light nuclei is presented. It uses an expansion in terms of Faddeev components for which the dynamic equations are derived. The model is designed to investigate binary channel processes in a compound system. Gaussian and oscillator bases are used to expand the wave function and to represent appropriate boundary conditions. We study the effect of cluster polarization on ground and resonance states of 7 Be, and on the astrophysical S-factor of the reaction 6 Li(p, 3 He) 4 He.

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Section: The Reaction 6 Li(p 3 He) 4 Hementioning

confidence: 96%

A microscopic three-cluster model with nuclear polarization applied to the resonances of 7Be and the reaction 6Li(p, 3He)4He

et al. 2009

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“…E.4 and E.6. The spallation of energetic freshly synthesized 6 Li reaction 84 has also been included [69] but plays only a minor role for the results.…”

Section: Nuclear Spallationmentioning

confidence: 99%

Big bang nucleosynthesis constraints on hadronically and electromagnetically decaying relic neutral particles

2006

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Big Bang nucleosynthesis in the presence of decaying relic neutral particles is examined in detail. All non-thermal processes important for the determination of light-element abundance yields of 2 H, 3 H, 3 He, 4 He, 6 Li, and 7 Li are coupled to the thermonuclear fusion reactions to obtain comparatively accurate results. Predicted light-element yields are compared to observationally inferred limits on primordial light-element abundances to infer constraints on the abundances and properties of relic decaying particles with decay times in the interval 0.01 sec < ∼ τX < ∼ 10 12 sec. Decaying particles are typically constrained at early times by 4 He or 2 H, at intermediate times by 6 Li, and at large times by the 3 He/ 2 H ratio. Constraints are shown for a large number of hadronic branching ratios and decaying particle masses and may be applied to constrain the evolution of the early Universe.

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“…In addition, we present the S-factor curve corresponding to the rate found in the compilation of Harris et al [12]. Following Engstler et al [10], we use only the data above 100 keV [13,14,15,16,17,18,19,20,10] in the fit to avoid the effects of electron screening. Unlike their fit, ours includes their data in addition to previous data.…”

Section: Hementioning

confidence: 99%

“…Experimental data for the reaction are shown, along with our fit (solid line), "1σ" and "2σ" uncertainties in our fit (symmetrical dot-dash lines), and the standard fit of Harris et al [12] (long dash line). Data are those of > Gemeinhardt [13], Fiedler & Kunze [15], < Spinka et al [16], ✷ Kwon et al [14], ✸ Shinozuka et al [17], ⋆ Elwyn et al [18], △ Marion et al [19], × Várnagy et al [20], and ▽ Engstler et al [10].…”

Section: Figmentioning

confidence: 99%

Nuclear reaction rates and primordial6Li

1997

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We examine the possibility that Big Bang Nucleosynthesis (BBN) may produce non-trivial amounts of 6 Li. If a primordial component of this isotope could be observed, it would provide a new fundamental test of Big-Bang cosmology, as well as new constraints on the baryon density of the universe. At present, however, theoretical predictions of the primordial 6 Li abundance are extremely uncertain due to difficulties in both theoretical estimates and experimental determinations of the 2 H(α, γ) 6 Li radiative capture reaction cross-section. We also argue that present observational capabilities do not yet allow the detection of primeval 6 Li in very metal-poor stars of the galactic halo. However, if the critical cross section is towards the upper end of its plausible range, then improvements in 6 Li detection capabilities may allow the establishment of 6 Li as another product of BBN. It is also noted that a primordial 6 Li detection could help resolve current concerns about the extragalactic D/H determination. 26.35.+c,26.44.+h,25.90.+k

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Cross sections for theLi6(p,

Cited by 45 publications

References 21 publications

A microscopic three-cluster model with nuclear polarization applied to the resonances of 7Be and the reaction 6Li(p, 3He)4He

A microscopic three-cluster model with nuclear polarization applied to the resonances of 7Be and the reaction 6Li(p, 3He)4He

Big bang nucleosynthesis constraints on hadronically and electromagnetically decaying relic neutral particles

Nuclear reaction rates and primordial6Li

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