Gamma-ray yields from the reaction D(p, γ)<sup>3</sup>He at low energies

Bailey, G.M.; Griffiths, G. M.; Olivo, M.; Helmer, R. L.

doi:10.1139/p70-379

Cited by 37 publications

(37 citation statements)

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“…The target gas composition is monitored with a mass spectrometer Q200, where the analyzed gas is reduced via a special pressure converter DWl Fig. This reaction proceeds [37][38][39][40] by the direct capture mechanism and represents a case similar to the 3He(~, y)7Be reaction. The pressure reduction in the jet target system along the accelerator beam axis (Fig.…”

Section: Jet-quality For 7-ray Spectroscopymentioning

confidence: 99%

“…4.1.1) the 3He(~, 7)TBe cross sections were measured relative to the well-known DC cross sections for the reactions D(p, y)3He [37][38][39][40] and ~60(p,~)lTF [14,57,58]. 4.1.1) the 3He(~, 7)TBe cross sections were measured relative to the well-known DC cross sections for the reactions D(p, y)3He [37][38][39][40] and ~60(p,~)lTF [14,57,58].…”

Section: I2 Cross Section Relative To Non-resonant Capture Reactimentioning

confidence: 99%

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The3He(?,?)7Be reaction and the solar neutrino problem

et al. 1982

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The capture reaction 3He(c~, y)TBe has been investigated in the energy range of E .... = 107 to 1,266 keV. The 4He or 3He beams of up to 300 gA particle current were incident on 3He or 4He gas targets, respectively. The gas target systems were all of the windowless and recirculating type. Excitation functions have been obtained with the use of an extended-static gas target, while the measurements of y-ray angular distributions involved a quasi-point supersonic jet system. The determination of absolute cross sections has been carried out with both types of gas target systems. The 7-ray yields in the 3He(~, 7)7Be reaction were detected using 80 cm 3 Ge(Li) detectors. The data lead to a zero-energy intercept of the astrophysical S(E) factor of S(0)=0.30+0.03 keV-b. This result reduces the calculated solar neutrino rate by a factor of 1.76.Nuclear Reactions: 3He(~, 7)7Be, E ..... = 107 to 1,266 keV; measured o-(E, E~,, 07.); deduced spectroscopic factors and astrophysical S-factor; solar neutrino problem; extended and quasi-point jet gas targets, Ge(Li) detectors.

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Section: Jet-quality For 7-ray Spectroscopymentioning

confidence: 99%

Section: I2 Cross Section Relative To Non-resonant Capture Reactimentioning

confidence: 99%

The3He(?,?)7Be reaction and the solar neutrino problem

et al. 1982

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“…Two previous studies of the H(p, y) He reaction have been made in the energy region of interest (E"~80 keV) [3,4]. Our rationale for restudying this reaction comes from the fact that the existing data set below 50 keV (Griffiths et al.…”

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confidence: 99%

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

et al. 1995

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The 2H(p, y) He reaction has been studied in the energy region E =80 -0 keV (E, =53,3 -0 keV), where the quantities measured were a(H, E) and A (//, E') Our res.ult for the total H(p, y) He 5 factor at E Oi=s S(0) =0.121~0.012 eV b (including systematic error), which is 52% lower than the presently accepted value. Some astrophysical aspects of this result are discussed. We have also extracted the El and M 1 S(E) components using our detailed angular distribution data. These data will provide sensitive tests for three-body calculations which include Coulomb and meson exchange current effects. PACS number(s): 25.40.Lw, 24.70.+s, 95.30.CqThe motivation to experimentally study the H(p, y) He reaction at low energies is twofold: first of all, to further test and refine the results of theoretical three-body calculations and second, to study the aspects of the H(p, y) He reaction which are of interest in astrophysics. The basic physics impetus for the current H(p, y) He work was provided by a recently published exact three-body calculation [1] for the tored to gauge changes in the purity of the D20 ice target (no problems were encountered). Figure 1(b) shows a blow up of the full energy peak (with the anticoincidence condition ap-0556-2813/95/52(4)/1732(4)/$06. 00

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“…There are several data sets for this reaction in the BBN window: however, some of these measurements need detailed consideration. It has been suggested that the Griffiths'63 [5] and Bailey'70 [6] experiments used incorrect stopping powers and, consequently, their low energy behaviour is 15% too high. The Schmid'97 [7] data set suffer from poor energy resolution, with typical uncertainties greater than 10%.…”

Section: Existing Experimental Datamentioning

confidence: 99%

Towards the study of²H(p, γ)³He reaction in the Big Bang Nucleosynthesis energy range in LUNA

Kochanek

2016

J. Phys.: Conf. Ser.

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Abstract. The Big Bang Nucleosynthesis began a few minutes after the Big Bang, when the Universe was sufficiently cold to allow deuterium nuclei to survive photo-disintegration. The total amount of deuterium produced in the Universe during the first minutes depends on the cosmological parameters (like the energy density in baryons, Ω b h 2 , and the effective neutrino number, N ef f ) and on the nuclear cross sections of the relevant reactions. The main source of uncertainty in the deuterium estimation comes from the 2 H(p, γ) 3 He cross section. Measurements of Cosmic Microwave Background (CMB) anisotropies obtained by the Planck satellite are in very good agreement with the theoretical predictions of the minimal ΛCDM cosmological model, significantly reducing the uncertainty on its parameters. The Planck data allows to indirectly deduce with very high precision the abundances of primodial nuclides, such as the primodial deuterium fraction 2 H/H = (2.65 ± 0.07) · 10 −5 (68% C.L.). The astrophysical observations in damped Lyman-α systems at high redshifts provide a second high accuracy measurement of the primodial abundance of deuterium 2 H/H = (2.53 ± 0.04) · 10 −5 (68% C.L.). The present experimental status on the astrophysical S-factor of the 2 H(p, γ) 3 He reaction in the BBN energy range, gives a systematic uncertainties of 9%. Also the difference between ab-initio calculations and experimental values of S12 is at the level of 10%. In order to clarify the actual scenario, a measurement of 2 H(p, γ) 3 He cross section with a precision of a few percent in the 70-400 keV energy range is planned at LUNA in 2016. A feasibility test of the measurement has been performed in October 2014, giving the preliminary results on the cross section. The experimental setup for the test and final measurement campaign will be presented.

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Gamma-ray yields from the reaction D(p, γ)³He at low energies

Abstract: Total cross sections and measurements of the small isotropic component of the γ-ray yield from the reaction D(p, γ)3He have been determined in the energy range from 57 to 1100 KeV using gas and deuterated polyethylene targets. The results are compared with some theoretical predictions.

Cited by 37 publications

References 0 publications

The3He(?,?)7Be reaction and the solar neutrino problem

The3He(?,?)7Be reaction and the solar neutrino problem

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

Towards the study of²H(p, γ)³He reaction in the Big Bang Nucleosynthesis energy range in LUNA

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Gamma-ray yields from the reaction D(p, γ)3He at low energies

Abstract: Total cross sections and measurements of the small isotropic component of the γ-ray yield from the reaction D(p, γ)3He have been determined in the energy range from 57 to 1100 KeV using gas and deuterated polyethylene targets. The results are compared with some theoretical predictions.

Cited by 37 publications

References 0 publications

The3He(?,?)7Be reaction and the solar neutrino problem

The3He(?,?)7Be reaction and the solar neutrino problem

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

Towards the study of2H(p, γ)3He reaction in the Big Bang Nucleosynthesis energy range in LUNA

Contact Info

Product

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About

Gamma-ray yields from the reaction D(p, γ)³He at low energies

Towards the study of²H(p, γ)³He reaction in the Big Bang Nucleosynthesis energy range in LUNA