Characterizing the astrophysical 
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 factor for 
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 fusion with

Díaz-Torres, A.; Wiescher, M.

doi:10.1103/physrevc.97.055802

Cited by 50 publications

(42 citation statements)

References 48 publications

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“…Note, that for 12 C+ 12 C reaction the early measured data [6,13] differ from the later ones [14,22]. Here, the mechanism that causes the oscillations of the cross section in the 12 C+ 12 C reaction is not considered [25].…”

Section: Results Of Calculationsmentioning

confidence: 99%

Extended quantum diffusion approach to reactions of astrophysical interests

et al. 2020

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The quantum diffusion approach is extended to low energy fusion (capture) reactions of lightand medium-mass nuclei. The dependence of the friction parameter on bombarding energy is taken into account. A simple analytic expression is obtained for the capture probability at extreme subbarrier energies. The calculated cross-sections are in a good agreement with the experimental data. The fusion excitation functions calculated within the quantum diffusion and WKB approaches are compared and presented in the astrophysical S-factor representation.

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Section: Results Of Calculationsmentioning

confidence: 99%

Extended quantum diffusion approach to reactions of astrophysical interests

et al. 2020

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“…Alternatively, polarization effects can be included via the coupled-channels method based on a bare (energy-independent) nucleus-nucleus potential, e.g., calculated with a modified double-folding technique [18,19]. Deformation effects of 12 C have also been investigated with potential models [20], microscopic calculations [21], and the time-dependent wave-packet method in an attempt to reproduce the resonances that show in 12 C+ 12 C fusion [22].…”

Section: Introductionmentioning

confidence: 99%

Absence of hindrance in a microscopic C12+C12 fusion study

2019

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Background: Studies of low-energy fusion of light nuclei are important in astrophysical modeling, with small variations in reaction rates having a large impact on nucleosynthesis yields. Due to the lack of experimental data at astrophysical energies, extrapolation and microscopic methods are needed to model fusion probabilities. Purpose: To investigate deep sub-barrier 12 C+ 12 C fusion cross sections and establish trends for the S factor. Method: Microscopic methods based on static Hartree-Fock and time-dependent Hartree-Fock (TDHF) meanfield theory are used to obtain 12 C+ 12 C ion-ion fusion potentials. Fusion cross sections and astrophysical S factors are then calculated using the incoming wave boundary condition method. Results: Both density-constrained frozen Hartree-Fock (DCFHF) and density-constrained TDHF (DC-TDHF) predict a rising S factor at low energies, with DC-TDHF predicting a slight damping in the deep sub-barrier region (≈1 MeV). Comparison between DC-TDHF calculations and maximum experimental cross sections in the resonance peaks are good. However, the discrepancy in experimental low-energy results inhibits interpretation of the trend. Conclusions: Using the fully microscopic DCFHF and DC-TDHF methods, no S factor maximum is observed in the 12 C+ 12 C fusion reaction. In addition, no extreme sub-barrier hindrance is predicted at low energies. The development of a microscopic theory of fusion including resonance effects, as well as further experiments at lower energies must be done before the deep sub-barrier behavior of the reaction can be established.

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“…The presence of resonances in the 12 C þ 12 C reaction has been hotly debated for over 60 years. The conventional wisdom is that they correspond to the formation of shortlived molecular states [5,6], and this early suggestion has led on to far wider discussion of clustering in alphaconjugate systems [7][8][9][10][11][12]. However, this model remains controversial: an alternate picture [13] is that the resonant behavior is simply an artifact of the low level density of the 12 C þ 12 C compound system.…”

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Advances in the Direct Study of Carbon Burning in Massive Stars

Fruet¹,

Courtin²,

Heine³

et al. 2020

Phys. Rev. Lett.

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The 12 C þ 12 C fusion reaction plays a critical role in the evolution of massive stars and also strongly impacts various explosive astrophysical scenarios. The presence of resonances in this reaction at energies around and below the Coulomb barrier makes it impossible to carry out a simple extrapolation down to the Gamow window-the energy regime relevant to carbon burning in massive stars. The 12 C þ 12 C system forms a unique laboratory for challenging the contemporary picture of deep sub-barrier fusion (possible sub-barrier hindrance) and its interplay with nuclear structure (sub-barrier resonances). Here, we show that direct measurements of the 12 C þ 12 C fusion cross section may be made into the Gamow window using an advanced particle-gamma coincidence technique. The sensitivity of this technique effectively removes ambiguities in existing measurements made with gamma ray or charged-particle detection alone. The present cross-section data span over 8 orders of magnitude and support the fusion-hindrance model at deep sub-barrier energies.

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Characterizing the astrophysical S factor for C12+C12 fusion with

Cited by 50 publications

References 48 publications

Extended quantum diffusion approach to reactions of astrophysical interests

Extended quantum diffusion approach to reactions of astrophysical interests

Absence of hindrance in a microscopic C12+C12 fusion study

Advances in the Direct Study of Carbon Burning in Massive Stars

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