Helium burning

/ˈhiliəm ˈbɜrnɪŋ/ noun

The nuclear fusion process in evolved stars where helium nuclei combine to form heavier elements like carbon and oxygen. This occurs at much higher temperatures than hydrogen burning, typically above 100 million Kelvin.

From Greek 'helios' (sun, where helium was first detected) + 'burning' (from Old English 'byrnan'). The term developed in the mid-20th century as astronomers understood stellar nucleosynthesis processes.

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