Large-basis ab initio no-core shell model and its application to 12 C

By P. Navrátil, J. Vary, B. Barrett. 2000

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Nuclear weak-interaction processes in stars (2002, background): “These are currently only feasible for light nuclei where ab initio shell model calculations are possible (Caurier et al., 2001; Navrátil et al., 2000).”
The shell model as a unified view of nuclear structure (2004, methodology): “Another important NCSM indication is that the excitation spectra converge well before the full energy, which validates formally the 0ω diagonalizations with rudimentary potentials 9 and second order corrections.”
Double Beta Decay, Majorana Neutrinos, and Neutrino Mass (2007, background): “…and references therein), and controlled approximation schemes that treat all the nucleons with the same interactions (e.g. the no-core shell model (Navratil et al., 2000) and the coupled-clusters approach (Kowalski et al., 2004; Wloch et al., 2005)) currently work well for bound-state energies in…”
Microscopic clustering in light nuclei (2017, background): “The fact that no-core shell-model calculations fail to reproduce the energy of the Hoyle state (Navrátil, Vary, and Barrett, 2000b; Navrátil et al., 2007), without resorting to a significantly expanded harmonic oscillator basis, indicates already that the structure lies beyond that readily…”