Nucleosynthesis in the Big Bang and in Stars

Quantum diffusion description of the subbarrier-capture process in heavy-ion reactions

“…slightly below the Coulomb barrier was recently observed in experiments reported in [2][3][4][5][6]. In terms of the astrophysical S factor [7,8], S = E c.m. σ exp(2πη), where η(E c.m. )…”

“…A number of experimental studies devoted to the fusion of heavy ions at deep-subbarrier energies have been performed to date [1][2][3][4][5][6][7][8][9][10][11]. Data from those experiments are of interest in addressing astrophysical problems associated with nucleosynthesis.…”

Theoretical models in nuclearastrophysics

“…The S factor determined in this way (S E2 (300 keV) = 42 ± 2 keV-b) is slightly lower than a microscopic cluster calculation (50 keV-b) [45], but should be more reliable as all properties of the 2 + resonances are taken from experiment. 7 Be(p,γ) 8 …”

“…Theoretical models in nuclear astrophysics Pierre Descouvemont operator, is nothing but the overlap between the initial 7 Be+p and final 8 B wave functions, is in general overestimated by a cluster model. This overestimation factor decreases as the model is improved.…”

“…In most experiments, a microscopic cluster model [33] (hereafter referred to as DB94) is used for the extrapolation. This model takes account of the 7 Be deformation, of inelastic and rearrangement channels, and has been tested with spectroscopic properties of 8 B and 8 Li, as well as with the 7 Li(n,γ) 8 Li mirror cross section. An update of the calculation has been performed more recently [52].…”