The astrophysical S‐factor widely used in the literature is a linear or a second order polynomial fit in terms of energy. In this work, we assume an exponential form of the S‐factor. The S‐factor can then be written in the form ℓnS0 + f(E) where S0 = 5.523 MeV and f(E) = ax + bx2 + cx3. By fitting the experimental cross section for He3He3, we obtain a = −0.88, b = 0.59 and c = −0.11. We evolve a solar model and compare with those of the standard cross section compilation. Most of the physical and chemical profiles differ at most by a few percent but the He3 abundance is higher by 20 %. This might affect the Be7 and B8 neutrino productions.

This content is only available via PDF.
You do not currently have access to this content.