12C + 4He | → | 16O + γ |
16O + 4He | → | 20Ne + γ |
20Ne+ 4He | ↔ | 44Mg + γ |
All these reactions have a very low rate and therefore do not contribute significantly to the energy production in stars; with elements heavier than Neon (atomic number > 20) they occur even less easily due to the increasing Coulomb barrier[?].
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