Cross Section and Angular Distribution of the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msup><mml:mrow><mml:mi mathvariant="normal">He</mml:mi></mml:mrow><mml:mrow><mml:mn>3</mml:mn></mml:mrow></mml:msup></mml:mrow><mml:mn /><mml:mo>(</mml:mo><mml:mi>d</mml:mi><mml:mo>,</mml:mo><mml:mi>p</mml:mi><mml:mo>)</mml:mo><mml:mn /><mml:mrow><mml:msup><mml:mrow><mml:mi mathvariant="normal">He</mml:mi></mml:mrow><mml:mrow><mml:mn>4</mml:mn></mml:mrow></mml:msup></mml:mro

Bonner, T. W.; Conner, J. P.; Lillie, A. B.

doi:10.1103/physrev.88.473

Cited by 81 publications

(29 citation statements)

References 7 publications

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“…It is the second route to 4 He production after the tdn reaction, but its indetermination mainly plays a role in the 3 He and 7 Li yields, as it essentially controls the burning of 3 He. The data considered in our analysis are the ones reported in [112]- [125]; the two recent data sets [124,125], firstly included in this compilation, once corrected for the screening effect allow for a better coverage of the low-energy region. Our new rate agrees within the errors with the rate published in [14], where the total error is estimated to be 8% (1 σ).…”

Section: Reaction He3dpmentioning

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.

249

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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Section: Reaction He3dpmentioning

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.

249

307

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“…In the case of the Bonner et al measurement [59], this may be attributable to energy straggling in the gas target's Al window. In any case, there is little else to say here except to point out that our piecewise spline seems to represent the data about as well as the SKM R-matrix fit.…”

Section: He(d P) 4 Hementioning

confidence: 99%

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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“…For higher energies, low angular dependence of the 3 He(d, p) 4 He cross-section is observed by Yarnell et al [16] and Bonner et al [17]. They reported that the ratio of the proton yield detected at 0°by the proton yield obtained at 90°amounts to 1.07 and 1.04 for incident energy of 978 and 1140 keV, respectively.…”

Section: Cross-section Measurementsmentioning

confidence: 83%

“…There is indeed a large uncertainty in the value at the maximum of the cross-section. It differs by as much as 30% depending on the authors [13][14][15][16][17][18][19]. The results obtained by the coincidence technique show that the profile at depth over 1 lm can be resolved at a scale of 0.1 lm with a 3 He detection limit close to 0.01 at.% in 3 He implanted UO 2 .…”

Section: Introductionmentioning

confidence: 86%