Abstract
The behaviour of intermediate nuclei taking part in H-burning is analysed. Comparing time scales for equilibrium with the time scale of convective mixing, we find that Be7, C13, N15, O17 cannot be assumed everywhere asbona fide secondary elements in stellar evolutionary computations. Some consequences of the onset of CNO burning are also discussed.
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Castellani, V., Sacchetti, M. ‘Primary’ elements in H-burning. Astrophys Space Sci 53, 217–221 (1978). https://doi.org/10.1007/BF00645915
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DOI: https://doi.org/10.1007/BF00645915