Towards an ab initio description of the light-nuclei radiative captures

TL;DR

This paper presents a first-principles calculation of astrophysical radiative capture processes involving light nuclei using a no-core shell model with continuum and chiral interactions, providing insights into nuclear reactions relevant for astrophysics.

Contribution

It introduces an ab initio method to compute low-energy radiative capture S-factors for light nuclei, combining no-core shell model with continuum and renormalized chiral interactions.

Findings

Calculated S-factors for ${^3{ m He}}( ext{α}, ext{γ}){^7{ m Be}}$ and ${^3{ m H}}( ext{α}, ext{γ}){^7{ m Li}}$ at energies below 2.5 MeV.

Demonstrated the effectiveness of the no-core shell model with continuum approach for astrophysical reactions.

Provided results consistent with experimental data within theoretical uncertainties.

Abstract

The ${^3{\rm He}}(\alpha,\gamma){^7{\rm Be}}$ and ${^3{\rm H}}(\alpha,\gamma){^7{\rm Li}}$ astrophysical $S$ factors are evaluated at low collision energies (less than 2.5 MeV in the centre-of-mass frame) within the no-core shell model with continuum approach using a renormalized chiral nucleon-nucleon interaction.