Reexamination of the astrophysical<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mi>S</mml:mi></mml:mrow></mml:math>factor for the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mi>α</mml:mi></mml:mrow></mml:math>+<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mi>d</mml:mi><mml:mo>→</mml:mo><mml:msup><mml:mi /><mml:mrow><mml:mn>6</mml:mn></mml:mrow></mml:msup></mml:mrow></mml:math>Li

Mukhamedzhanov, A. M.; Blokhintsev, L.D.; Irgaziev, B. F.

doi:10.1103/physrevc.83.055805

Cited by 56 publications

(121 citation statements)

References 24 publications

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“…The thermonuclear reaction rate obtained based on our data is much lower than the previous rate by Caughlan and Fowler (CF88, [28] ) but also lower than all other previously reported thermonuclear reaction rates [15,27,29] (see Fig. 6 and Table 4 ).…”

Section: Thermonuclear Reaction Rate and Astrophysical Implicationscontrasting

confidence: 50%

“…The situation is very different for the E1 contribution which is only constrained by the present data, which were not available at the time of publication of recent theoretical curves [15,27] . In order to address this problem, the Hammache E1 curve is rescaled so that the sum of E1 and E2 curves matches the present data.…”

Section: Thermonuclear Reaction Rate and Astrophysical Implicationsmentioning

confidence: 91%

“…(For interpretation of the references to colour in this figure legend, the reader is referred to the web version of this article.) [27] ); NACRE-II (orange dot-dashed curve [14] ). The rate from the present work (red solid line, and shaded error band) is also shown.…”

Section: Thermonuclear Reaction Rate and Astrophysical Implicationsmentioning

confidence: 99%

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Big Bang 6 Li nucleosynthesis studied deep underground (LUNA collaboration)

Trezzi

Anders

Aliotta

et al. 2017

Astroparticle Physics

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a b s t r a c tThe correct prediction of the abundances of the light nuclides produced during the epoch of Big Bang Nucleosynthesis (BBN) is one of the main topics of modern cosmology. For many of the nuclear reactions that are relevant for this epoch, direct experimental cross section data are available, ushering the so-called "age of precision". The present work addresses an exception to this current status: the 2 H( α, γ ) 6 Li reaction that controls 6 Li production in the Big Bang. Recent controversial observations of 6 Li in metal-poor stars have heightened the interest in understanding primordial 6 Li production. If confirmed, these observations would lead to a second cosmological lithium problem, in addition to the well-known 7 Li problem. In the present work, the direct experimental cross section data on 2 H( α, γ ) 6 Li in the BBN energy range are reported. The measurement has been performed deep underground at the LUNA (Laboratory for Underground Nuclear Astrophysics) 400 kV accelerator in the Laboratori Nazionali del Gran Sasso, Italy. The cross section has been directly measured at the energies of interest for Big Bang Nucleosynthesis for the first time, at E cm = 80, 93, 120, and 133 keV. Based on the new data, the 2 H( α, γ ) 6 Li thermonuclear reaction rate has been derived. Our rate is even lower than previously reported, thus increasing the discrepancy between predicted Big Bang 6 Li abundance and the amount of primordial 6 Li inferred from observations.

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Section: Thermonuclear Reaction Rate and Astrophysical Implicationscontrasting

confidence: 50%

Section: Thermonuclear Reaction Rate and Astrophysical Implicationsmentioning

confidence: 91%

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Big Bang 6 Li nucleosynthesis studied deep underground (LUNA collaboration)

Trezzi

Anders

Aliotta

et al. 2017

Astroparticle Physics

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“…The available data on the values of the ANCs C l and the NVCs G l for that channel are characterized by a large spread, especially for l = 2 (l = 0, 2 is the channel orbital angular momentum). The information on these data can be found in [3,7] and in references therein. In the present approach several sets of scattering phases obtained from the phase-shift analyses of dα scattering [8,9] as well as from the Faddeev calculations [3] are used as the input.…”

Section: Methods and Resultsmentioning

confidence: 99%

Analytic continuation of scattering data as a method of obtaining characteristics of bound states

Blokhintsev

Savin

2014

EPJ Web of Conferences

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Abstract. The method of the analytic continuation of the effective range function is applied to obtain the asymptotic normalization coefficients for 6 Li nucleus in the α+d channel. Several sets of scattering phases obtained from the phase-shift analyses as well as from Faddeev calculations are used as an input. Since the α+d system possesses the low-lying inelastic threshold due to the dissociation of a deuteron, the approach used is generalized to include inelastic channels. The sensitivity of the obtained values of asymptotic normalization coefficients to the elastic channels coupling and to account of the inelastic channel is investigated.

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“…Hence the amplitudes of the peripheral processes are proportional to the corresponding ANCs. That is why the ANC determines the overall normalization of the peripheral process amplitude [2,5]. Evidently that the ANC plays a crucial role in determination of other nuclear characteristics to calculate which we need to know the tail of the overlap function.…”

Section: Introductionmentioning

confidence: 99%

Asymptotic normalization coefficients and radiative widths

Mukhamedzhanov

Pang

2015

Phys. Rev. C

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Asymptotic normalization coefficent (ANC) is important quantity in calculation of the radiative width amplitudes providing limits on the radiative width. Here we present some examples showing connection between the ANC and radiative width. In particular, the radiative width of the E1Phys. A 217, 29 (1973) ] is (1.2 ± 0.2) × 10 −2 eV. Meantime the ANC for the first excited state in 17 F puts a low limit on the radiative width, which is (3.4 ± 0.50) × 10 −2 eV. Such a strong disagreement between the measured radiative width and the low limit imposed by the ANC calls for a new measurement of this radiative widh. Other examples are also considered.

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Reexamination of the astrophysicalSfactor for theα+d→6Li

Cited by 56 publications

References 24 publications

Big Bang 6 Li nucleosynthesis studied deep underground (LUNA collaboration)

Big Bang 6 Li nucleosynthesis studied deep underground (LUNA collaboration)

Analytic continuation of scattering data as a method of obtaining characteristics of bound states

Asymptotic normalization coefficients and radiative widths

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