Polarized proton capture by deuterium and the<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>2</mml:mn></mml:mrow><mml:mrow /><mml:mrow /></mml:mmultiscripts></mml:mrow><mml:mo>(</mml:mo><mml:mi>p</mml:mi><mml:mo>,</mml:mo><mml:mi> </mml:mi><mml:mi>γ</mml:mi><mml:mo>)</mml:mo><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi mathvariant="normal">He

Schmid, G. J.; Chasteler, R. M.; Laymon, C. M.; Weller, H.R.; Prior, R. M.

doi:10.1103/physrevc.52.r1732

Cited by 42 publications

(56 citation statements)

References 20 publications

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“…The previous measurements by the same authors gave 1.21(12)·10 −4 keV b [24] and the value 1.85(5)·10 −4 keV b was received in [25]. The average of these experimental measurements equals 1.69(58) · 10 −4 keV b what is in a good agreement with the value 1.65(5) · 10 −4 keV b calculated here only on the basis of the E1 transition.…”

mentioning

confidence: 73%

Astrophysical S -factor of p2H radiative capture

Dubovichenko

Dzhazairov-Kakhramanov

2009

Eur. Phys. J. A

179

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Abstract. The astrophysical S-factor of p 2 H radiative capture in the energy range down to 1 keV is considered in the potential cluster model with the classification of orbital states according to Young's scheme symmetry. It is shown that the approach used, which takes into account the E1 transition only, gives a good description of the new experimental data for two potentials of the bound state of the The radiative p + 2 H → 3 He + γ capture is a part of the hydrogen cycle and gives a considerable contribution to the energy efficiency of thermonuclear reactions [1] which account for burning of the Sun and stars of our Universe. The interacting nuclear particles of the hydrogen cycle have a minimal value which is a potential barrier. Thus, it is the first chain of nuclear reactions which can take place at ultralow energies and star temperatures. Then, for this chain, the process of the radiative p 2 H capture is the basic process for the transition from the primary proton fusion p + p → 2 H + e − + ν e to the final process 3 He+ 3 He → 4 He+2p [2] in the p-p chain. That is why the theoretical and experimental investigation of the radiative p 2 H capture in detail is of fundamental interest not only for nuclear astrophysics, but also for nuclear physics of ultralow energies and lightest atomic nuclei.We will discuss the astrophysical S-factors on the basis of a potential cluster model which takes into account the supermultiplet symmetry of wave functions (WF) with the splitting of orbital states according to Young's schemes. This approach allows us to analyse the structure of inter-cluster interactions, detecting allowed and forbidden states in the interaction potential, and thus, the number of WF nodes of the relative motion of clusters [3,4].The total cross-sections of the photoprocesses of the lightest nuclei were considered in this approach in our work [4]. E1 transitions resulting from the orbital part of the electric operator Q Jm (L) were taken into account in these calculations of the photodecays of 3 He and 3 H a e-mail: albert-j@yandex.ru nuclei into p 2 H and n 2 H channels. The values of E2 crosssections and cross-sections depending on the spin part of the electric operator turned out to be several times less. Further, it was assumed that E1 electric transitions in the N 2 H system are possible between the "pure" (scheme {3}) 2 S state of 3 H and 3 He nuclei and the doublet 2 P scattering state mixed according to Young's schemes {3} + {21}.To calculate photonuclear processes in the systems under consideration the nuclear part of the potential of intercluster p 2 H and n 2 H interactions is represented aswith a point-like Coulomb potential, V 0 -the Gaussian attractive part, and V 1 -the exponential repulsive part. The potential of each partial wave was constructed so that it would correctly describe the respective partial phase shift of the elastic scattering [5]. Using this concept, the potentials of the p 2 H interaction for scattering processes were received, parameters of such potentials were ful...

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mentioning

confidence: 73%

Astrophysical S -factor of p2H radiative capture

Dubovichenko

Dzhazairov-Kakhramanov

2009

Eur. Phys. J. A

179

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“…Some discrepancies exist for the lower energies data, but in [90] the authors stress on the presence of a systematic error in their previous data (see e.g. [89]), with an upward correction that reduces the compatibility problem with the older data reported in [92]. Moreover, the latter data set by Griffiths is likely to be affected by a 10%-15% normalization error due to the wrong stopping powers used for the heavy-ice targets [91,93], so that the disagreement is now reduced with respect to the first claims.…”

Section: Reaction Dpγmentioning

confidence: 98%

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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“…In the following, we detail the experimental data that we considered in this evaluation, in general taken from published tables, but when scanned from a figure, we provide here tables of the extracted numerical values. It was found, that NACRE overlooked the overall scaling factor of 1.37 [103] missing in the Schmidt et al [31] data. Here, we follow DAACV and use instead A 0 (multiplied by 4π) from Table II in Schmidt et al [36].…”

Section: Appendix B: the D(pγ)mentioning

confidence: 99%

“…[24][25][26][27][28][29][30][31][32][33], plus a few high energy experiments and a polynomial fit, while Descouvemont et al [15] (DAACV hereafter) used a slightly different set of data, from Refs. [21,[24][25][26][32][33][34][35][36] and included the data from Ref.…”

Section: The D(pγ)mentioning

confidence: 99%

New reaction rates for improved primordialD/Hcalculation and the cosmic evolution of deuterium

et al. 2015

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Primordial or big bang nucleosynthesis (BBN) is one of the three historical strong evidences for the big bang model. Standard BBN is now a parameter free theory, since the baryonic density of the Universe has been deduced with an unprecedented precision from observations of the anisotropies of the cosmic microwave background (CMB) radiation. There is a good agreement between the primordial abundances of 4 He, D, 3 He and 7 Li deduced from observations and from primordial nucleosynthesis calculations. However, the 7 Li calculated abundance is significantly higher than the one deduced from spectroscopic observations and remains an open problem. In addition, recent deuterium observations have drastically reduced the uncertainty on D/H, to reach a value of 1.6%. It needs to be matched by BBN predictions whose precision is now limited by thermonuclear reaction rate uncertainties. This is especially important as many attempts to reconcile Li observations with models lead to an increased D prediction. Here, we re-evaluates the d(p,γ) 3 He, d(d,n) 3 He and d (d,p) 3 H reaction rates that govern deuterium destruction, incorporating new experimental data and carefully accounting for systematic uncertainties. Contrary to previous evaluations, we use theoretical ab initio models for the energy dependence of the S-factors. As a result, these rates increase at BBN temperatures, leading to a reduced value of D/H = (2.45±0.10) × 10 −5 (2σ), in agreement with observations.

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Polarized proton capture by deuterium and theH2(p, γ)He

Cited by 42 publications

References 20 publications

Astrophysical S -factor of p2H radiative capture

Astrophysical S -factor of p2H radiative capture

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

New reaction rates for improved primordialD/Hcalculation and the cosmic evolution of deuterium

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