Speaker
Description
In the standard Big Bang Nucleosynthesis (BBN) framework, the primitive ${^6{Li}}$ abundance is mainly determined by two nuclear reactions: the
$d(\alpha,\gamma ){^6{Li}}$ reaction, where deuteron reacts with an alpha particle to produce ${^6{Li}}$. This reaction leads to the formation of ${^6{Li}}$ during the primordial nucleosynthesis process. Conversely, ${^6{Li}}(p,\alpha ){^3{He}}$, can destroy ${^6{Li}}$ and reduces the abundance of ${^6{Li}}$ in the early universe. In this study, we focused on the radiative capture process of the deuteron on alpha leading to the formation of $^6{{Li}}$ through the cluster Effective Field Theory. The contribution of the Coulomb interaction between particles was taken into account nonpurbatively. In the first step, the asymptotic normalization coefficients (ANCs) of the bound state of $^6{{Li}}$ was calculated based on the elastic scattering process of the alpha-deuteron system. In the following, the calculation of the transition amplitude and astrophysical S-factor were outlined. To evaluate the accuracy of the approach, we compare the astrophysical S-factor of the dominant electromagnetic transitions (E1 and E2) up to next-to-leading order with the experimental data.
