Radiative 3He(2H, γ)5Li capture at astrophysical energy and its role in accumulation of 6Li at the BBN

Abstract

Abstract Big Bang Nucleosynthesis (BBN) relevance reactions 3He(2H, γ)5Li, 3H(3He, γ)6Li, and 5Li(n, γ)6Li as a key to approach for scenario of 6Li formation are treated. The rates of reaction for these processes are analyzed. Comparison of the reactions rates and the prevalence of light elements leads to the assumption that the two-step process 2H + 3He → 5 Li + γ and n + 5Li → 6 Li + γ can make a significant contribution to the formation of 6Li at the BBN at least at temperatures T 9 of the order of unity. Calculations of the total cross sections, astrophysical S-factor, and reaction rates have been performed for 3He(2H, γ)5Li radiative capture within the modified potential cluster model with forbidden states, which follow from the classification of the orbital cluster states according to Young diagrams. Numerical data and corresponding parametrizations cover the energy range up to 5 MeV and temperature range T 9