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Hahn, K. I.; Brune, C. R.; Kavanagh, R. W.

doi:10.1103/physrevc.51.1624

Cited by 33 publications

(59 citation statements)

References 34 publications

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“…The S-factor is equal to 1.1(1)⋅10 -3 keV⋅b at energy of 1 keV, and its calculated value at energy of 50 keV is slightly less than S(0) = 2.0(2)⋅10 -3 keV⋅b reported in [28]. We note that simple extrapolation of the experimental data to 1 keV based on the three last points reported in [26,27] yields 0.6(2)⋅10 -3 keV⋅b, that is, three times smaller than in [28].…”

Section: Introductionmentioning

confidence: 55%

“…The experimental data were taken from [25]; by the time of calculations, they were known only for energies exceeding 700 keV. More recently, new experimental data on the S-factor at energies down to 12 keV were published in [26][27][28]. They are also shown in Fig.…”

Section: Introductionmentioning

confidence: 99%

“…Its values calculated for two asymptotes at distances of 8-16 fm were С 0 = 4.1(1) and С w = 4.6(1); according to [13], its experimental value ranged from 4.2 to 5.1. Here squares show experimental data taken from [25], closed circles from [26], triangles from [27], and open circles from [28].…”

Section: Introductionmentioning

confidence: 99%

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Astrophysical S-factors for р 2Н and р 3Н radiative capture

Dubovichenko

2009

Russ Phys J

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Section: Introductionmentioning

confidence: 55%

Section: Introductionmentioning

confidence: 99%

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Astrophysical S-factors for р 2Н and р 3Н radiative capture

Dubovichenko

2009

Russ Phys J

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“…We have omitted the Coulomb-breakup measurement of Utsunomiya et al [77] because the Coulomb-breakup process is not completely understood for this reaction (as discussed in SKM) and because the cross section energy dependence derived from this method disagrees with the Brune et al data. We note that the problem with normalization of the Schröder et al [74] and Griffiths et al [75] data sets mentioned by SKM seems to have gone away in the intervening time [78]. …”

Section: T(α γ) 7 LImentioning

confidence: 74%

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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“…The old rate for this reaction is that published in the compilation [12]. Meanwhile, new data were taken [158,159], and a new fitting of the astrophysical S factor is now available [159] S(E)…”

Section: Reaction Tpγmentioning

confidence: 99%

Nuclear reaction network for primordial nucleosynthesis: a detailed analysis of rates, uncertainties and light nuclei yields

Serpico

Esposito

Iocco

et al. 2004

J. Cosmol. Astropart. Phys.

250

307

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Abstract. We analyze in details the standard Primordial Nucleosynthesis scenario. In particular we discuss the key theoretical issues which are involved in a detailed prediction of light nuclide abundances, as the weak reaction rates, neutrino decoupling and nuclear rate modeling. We also perform a new analysis of available data on the main nuclear processes entering the nucleosynthesis reaction network, with particular stress on their uncertainties as well as on their role in determining the corresponding uncertainties on light nuclide theoretical estimates. The current status of theoretical versus experimental results for 2 H, 3 He, 4 He and 7 Li is then discussed using the determination of the baryon density as obtained from Cosmic Microwave Background anisotropies.

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H3(p,γ)4

Cited by 33 publications

References 34 publications

Astrophysical S-factors for р 2Н and р 3Н radiative capture

Astrophysical S-factors for р 2Н and р 3Н radiative capture

Estimating reaction rates and uncertainties for primordial nucleosynthesis

Nuclear reaction network for primordial nucleosynthesis: a detailed analysis of rates, uncertainties and light nuclei yields

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