<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi mathvariant="normal">H</mml:mi></mml:mrow><mml:mprescripts /><mml:mrow /><mml:mrow><mml:mn>3</mml:mn></mml:mrow><mml:mrow /><mml:mrow /></mml:mmultiscripts></mml:mrow></mml:math>(α,γ<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msup><mml:mrow><mml:mo>)</mml:mo></mml:mrow><mml:mrow><mml:mn>7</mml:mn></mml:mrow></mml:msup></mml:mrow></mml:math>Li

Brune, C. R.; Kavanagh, R. W.; Rolfs, C.

doi:10.1103/physrevc.50.2205

Cited by 94 publications

(121 citation statements)

References 41 publications

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“…A precise new measurement of the cross section for this process has been completed by Brune et al [14] in the time since the publication of SKM. Some subsequent calculations have incorporated the reaction rate derived from that measurement by its authors (e.g., Copi et al [1]), using as the uncertainty the 6% uncertainty in the experiment's cross section normalization.…”

Section: T(α γ) 7 LImentioning

confidence: 99%

“…Some subsequent BBN calculations (e.g., Ref. [1]) have incorporated the latest measurement of t(α, γ) 7 Li [14] by replacing the SKM fit with a reaction rate and uncertainty based on that measurement alone. These numbers have not found their way into all subsequent work (e.g., Ref.…”

Section: A the Databasementioning

confidence: 99%

“…This was a landmark work because it examined all the nuclear inputs critically and in detail, and it placed quantitative error estimates on all the inputs. There has been a small number of new cross section measurements since [14][15][16][17], which have been unevenly incorporated in subsequent work. Subsequent authors have continued to use the SKM rates and errors for most or all reactions.…”

Section: Introductionmentioning

confidence: 99%

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Estimating reaction rates and uncertainties for primordial nucleosynthesis

2000

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We present a Monte Carlo method for direct incorporation of nuclear inputs in primordial nucleosynthesis calculations. This method is intended to remedy shortcomings of current error estimation, by eliminating intermediate data evaluations and working directly with experimental data, allowing error estimation based solely on published experimental uncertainties. This technique also allows simple incorporation of new data and reduction of errors with the introduction of more precise data. Application of our method indicates that previous error estimates on the calculated abundances were too large by as much as a factor of three. Since uncertainties in the BBN calculation currently dominate inferences drawn from light-element abundances, the re-estimated errors have important consequences for cosmic baryon density, neutrino physics, and lithium depletion in halo stars. Our direct method allows detailed discussion of the status of the nuclear inputs, by identifying clearly the places where improved cross section measurements would be most useful. 26.35.+c, 98.80.Ft

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Section: T(α γ) 7 LImentioning

confidence: 99%

Section: A the Databasementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Estimating reaction rates and uncertainties for primordial nucleosynthesis

2000

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“…In summary, our calculations used the SKM rates, with α variation estimated as described above, and with updates from Refs. [27,28,29]. We compared a calculation using these rates and α BBN = α 0 with the corresponding results from the NACRE [30] and Nollett & Burles [31] evaluations of the rates (which are not suited to computing α variation).…”

Section: Laboratory Ratesmentioning

confidence: 99%

“…In the time since SKM (1993), some of the most uncertain cross sections have been remeasured. Newer, better rates exist for the processes d(p, γ) 3 He [26,27], t(α, γ) 7 Li [28], and 3 He(n, p) 3 H [29]. The revised rate for the first reaction has the usual functional form derived by the S-factor formalism (though its parameters are actually fitted to a numerical integration), and the expression from BIR, as corrected in Sec.…”

Section: Laboratory Ratesmentioning

confidence: 99%

Primordial nucleosynthesis with a varying fine structure constant: An improved estimate

Nollett

Lopez

2002

Phys. Rev. D

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We compute primordial light-element abundances for cases with fine structure constant α different from the present value, including many sources of α dependence neglected in previous calculations. Specifically, we consider contributions arising from Coulomb barrier penetration, photon coupling to nuclear currents, and the electromagnetic components of nuclear masses. We find the primordial abundances to depend more weakly on α than previously estimated, by up to a factor of 2 in the case of 7 Li. We discuss the constraints on variations in α from the individual abundance measurements and the uncertainties affecting these constraints. While the present best measurements of primordial D/H, 4 He/H, and 7 Li/H may be reconciled pairwise by adjusting α and the universal baryon density, no value of α allows all three to be accommodated simultaneously without consideration of systematic error. The combination of measured abundances with observations of acoustic peaks in the cosmic microwave background favors no change in α within the uncertainties.PACS numbers: 26.35.+c,98.80Ft,98.80.Es

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Ab Initio Nuclear Reaction Theory with Applications to Astrophysics

Navrátil

Quaglioni

2022

Handbook of Nuclear Physics

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H3(α,γ)7Li

Cited by 94 publications

References 41 publications

Estimating reaction rates and uncertainties for primordial nucleosynthesis

Estimating reaction rates and uncertainties for primordial nucleosynthesis

Primordial nucleosynthesis with a varying fine structure constant: An improved estimate

Ab Initio Nuclear Reaction Theory with Applications to Astrophysics

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