would follow from processes outlined by the B²FH paper. Clayton calculated the first time-dependent models of the ''s''-process in 1961 and of the ''r''-process in 1965, as well as of the burning of silicon into the abundant alpha-particle nuclei and iron-group elements in 1968, and discovered radiogenic chronologies for determining the age of the elements.

Key reactions

The most important reactions in stellar nucleosynthesis:
* Hydrogen

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