Extended parameterization of nuclear-reaction cross sections for few-nucleon nuclei

Chulick, G. S.; Kim, Y.E.; Rice, R. A.; Rabinowitz, Mario

doi:10.1016/0375-9474(93)90481-c

Cited by 34 publications

(17 citation statements)

References 57 publications

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“…For these and other reasons, these reactions have been studied over a wide range of center-of-mass energies E (E= 3.0 keV to 30 MeV), where the available data reported by various groups [5][6][7][8] agree rather well (within 10%).…”

Section: Introduction the D(dp)t And D(d N)3he Fusion Reactions (Inmentioning

confidence: 86%

Oppenheimer-Phillips effect and electron screening ind+ d fusion reactions

Greife

Gorris

Junker

et al. 1995

Z. Physik A - Hadrons and Nuclei

169

130

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Abstract. The d(d,n)3He and d(d,p)t fusion reactionshave been studied at center-of-mass energies E = 1.6 to 130 keV using intense beam currents from 30, 100, and 450 kV accelerators in combination with detectors in close and far geometry. The cross sesction ratio, (d,p), approaches unity (within 2%) at low energies; thus there is no experimental evidence for the Oppenheimer-Phillips effect at subcoulomb energies. R(E)=a(d,n)/cr The cross sections of d(d,p)t at E<10 keV show clearevidence for electron screening effects. However, the observed cross section enhancement is significantly larger than can be accounted for from available atomic physics models.

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Section: Introduction the D(dp)t And D(d N)3he Fusion Reactions (Inmentioning

confidence: 86%

Oppenheimer-Phillips effect and electron screening ind+ d fusion reactions

Greife

Gorris

Junker

et al. 1995

Z. Physik A - Hadrons and Nuclei

169

130

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“…The cross section data, now attributed to the effective energy E ′ , are then transformed into astrophysical S-factors S(E ′ ). For the exponent in the Gamow factor we used 2πη(E) = 68.75/ (E) (with E in keV), in accordance with [4,16]. As expected, the new astrophysical S-factors are significantly smaller than those reported in [4,7] (Fig.…”

mentioning

confidence: 83%

“…As in [7] we used the 3-rd order polynomial (n = 3) parametrization given in [16] for the bare-nuclei cross section. We find U e = 117 ± 7 eV with a χ 2 -value of 0.5 per degree of freedom.…”

mentioning

confidence: 99%

Energy loss, electron screening and the astrophysical 3He(d, p)4He cross section

et al. 1996

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We reanalyze the low-energy 3 He(d,p) 4 He cross section measurements of Engstler et al. using recently measured energy loss data for proton and deuteron beams in a helium gas. Although the new 3 He(d,p) 4 He astrophysical S-factors are significantly lower than those reported by Engstler et al., they clearly show the presence of electron screening effects. From the new astrophysical S-factors we find an electron screening energy in agreement with the adiabatic limit.The penetration through the Coulomb barrier forces the (non-resonant) cross section σ(E) between charged particles to drop exponentially with decreasing energy E. (Energies are in the center-of-mass system throughout this paper.) As a consequence, the cross section at the very low energies at which stellar hydrostatic burning takes place is in most cases too small to be measured directly in the laboratory. It is therefore customary in nuclear astrophysics to measure cross sections to energies as low as possible and then to extrapolate the data to the energy appropriate for the astrophysical application. Conventionally this extrap-

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“…Figure 11 shows the final two-body cross section as obtained in the present work (solid symbols) together with the direct data (open symbols) [61][62][63][64][65] used for the normalization procedure. The very good agreement between the two data sets confirms the usefulness of the MPWBA analysis in correctly describing the studied process at low energies.…”

Section: From the Qf Coincidence Data To The Indirect Two-body Cromentioning

confidence: 99%

Bare-nucleus astrophysical factor of theHe3(d,p)<

et al. 2005

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The 3 He (d, p) 4 He reaction has been studied from E c.m. = 600 keV down to astrophysical energies by means of the "Trojan horse" method using the 6 Li( 3 He,pα) 4 He three-body reaction at E lab = 5 and 6 MeV. Coincidence spectra were measured in kinematic conditions favoring the quasifree 3 He + 2 H process. The bare astrophysical factor S b (E) for the 3 He(d, p) 4 He reaction was extracted from the three-body cross section in the modified plane-wave Born approximation. Comparison with the S b extrapolation from the free two-body data is presented. The independent estimate of the screening potential as obtained with the present work seems to confirm the theoretical adiabatic limit.

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Extended parameterization of nuclear-reaction cross sections for few-nucleon nuclei

Cited by 34 publications

References 57 publications

Oppenheimer-Phillips effect and electron screening ind+ d fusion reactions

Oppenheimer-Phillips effect and electron screening ind+ d fusion reactions

Energy loss, electron screening and the astrophysical 3He(d, p)4He cross section

Bare-nucleus astrophysical factor of theHe3(d,p)<

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