Stellar nucleosynthesis is the collective term for the nuclear reactions taking place in stars to build the nuclei of the heavier elements.
The processes involved began to be understood early in the twentieth century, when it was first realised that the energy released from nuclear reactions accounted for the longevity of the Sun as a source of heat and light.
The prime energy producer in the sun is the fusion of hydrogen to helium, which occurs at a minimum temperature of 3 million kelvin.
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