Atomic effects in the determination of nuclear cross sections of astrophysical interest

Bracci, L.; Fiorentini, G.; Melezhik, Vladimir S.; Mezzorani, G.; Quarati, Piero

doi:10.1016/0375-9474(90)90101-q

Cited by 81 publications

(79 citation statements)

References 11 publications

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“…(33) and (37) with the ones obtained in Ref. [16]. For a reaction p + A Z X between a bare proton p and neutral atom A Z X we obtain: Table I.…”

Section: Multi-electron Screening Effectssupporting

confidence: 64%

“…(33) practically reproduces the sudden limit U SL e of Ref. [16], while Eq. (37) gives a higher adiabatic limit than the one U AL e given in Ref.…”

Section: Multi-electron Screening Effectsmentioning

confidence: 54%

“…(37) gives a higher adiabatic limit than the one U AL e given in Ref. [16]. Despite the fact that for the reaction 3 He ( 3 He, 2p) 4 He the electrons involved are too few to justify use of the above formulas it will give a sense of the validity of the present models if we apply our formulas on that reaction as well.…”

Section: Multi-electron Screening Effectsmentioning

confidence: 69%

“…Although the adiabatic limit [15,16] is generally accepted, in a recent paper [17] a simple and efficient model was proposed for the study of the screening effect on low-energy nuclear fusion reactions which exceeded that limit. In that model, the fusing atoms were considered hydrogen-like atoms whose electron probability density was used in Poisson's equation in order to derive the corresponding screened Coulomb potential energy.…”

Section: Introductionmentioning

confidence: 99%

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Atomic effects in astrophysical nuclear reactions

Liolios

2001

Phys. Rev. C

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Two models are presented for the description of the electron screening effects that appear in laboratory nuclear reactions at astrophysical energies. The two-electron screening energy of the first model agrees very well with the recent LUNA experimental result for the break-up reaction 3 He 3 He, 2p4 He, which so far defies all available theoretical models. Moreover, multi-electron effects that enhance laboratory reactions of the CNO cycle and other advanced nuclear burning stages, are also studied by means of the ThomasFermi model, deriving analytical formulae that establish a lower and upper limit for the associated screening energy. The results of the second model, which show a very satisfactory compatibility with the adiabatic approximation ones, are expected to be particularly useful in future experiments for a more accurate determination of the CNO astrophysical factors. PACS number(s): 25.10.+s, 25.55.-e, 25.45.-z,26.65.+t

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“…(33) and (37) with the ones obtained in Ref. [16]. For a reaction p + A Z X between a bare proton p and neutral atom A Z X we obtain: Table I.…”

Section: Multi-electron Screening Effectssupporting

confidence: 64%

“…(33) practically reproduces the sudden limit U SL e of Ref. [16], while Eq. (37) gives a higher adiabatic limit than the one U AL e given in Ref.…”

Section: Multi-electron Screening Effectsmentioning

confidence: 54%

Section: Multi-electron Screening Effectsmentioning

confidence: 69%

Section: Introductionmentioning

confidence: 99%

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Atomic effects in astrophysical nuclear reactions

Liolios

2001

Phys. Rev. C

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“…However that assumption is an oversimplification which will be amended in the present paper. The most sophisticated approach has been a few-body treatment [8] which established a lower (sudden) and a higher (adiabatic) limit for the screening energy transferred into the relative nuclear motion. Although more studies followed [9] [10], which also extended the calculations to molecular fusion reactions [11], despite their mathematical rigor they could not explain the discrepancy between experimental and theoretical screening energies.…”

Section: Introductionmentioning

confidence: 99%

Screened Coulomb potentials for astrophysical nuclear fusion reactions

Liolios

2000

Eur Phys J A

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The electron-screening acceleration of laboratory fusion reactions at astrophysical energies is an unsolved problem of great importance to astrophysics. That effect is modeled here by considering the fusion of hydrogen-like atoms whose electron probability density is used in Poisson's equation in order to derive the corresponding screened Coulomb potential energy. That way atomic excitations and deformations of the fusing atoms can be taken into account. Those potentials are then treated semiclassically in order to obtain the screening (accelerating) factor of the reaction. By means of the proposed model the effect of a superstrong magnetic field on laboratory Hydrogen fusion reactions is investigated here for the first time showing that, despite the considerable increase in the cross section of the dd reaction, the pp reaction is still too slow to justify experimentation. The proposed model is finally applied on the H 2 (d, p) H 3 fusion reaction describing satisfactorily the experimental data although some ambiguity remains regarding the molecular nature of the deuteron target. Notably, the present method gives a sufficiently high screening energy for Hydrogen fusion reactions so that the take-away energy of the spectator nucleus can also be taken into account. PACS number(s): 25.10.+s, 25.45.-z

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Influence of chaos on the fusion enhancement by electron screening

Kimura¹,

Bonasera²,

Cavallaro³

The 2nd International Conference on Nuclear Physics in Astrophysics

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Atomic effects in the determination of nuclear cross sections of astrophysical interest

Cited by 81 publications

References 11 publications

Atomic effects in astrophysical nuclear reactions

Atomic effects in astrophysical nuclear reactions

Screened Coulomb potentials for astrophysical nuclear fusion reactions

Influence of chaos on the fusion enhancement by electron screening

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