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Nuclear fusion produces certain isotopes of the lighter elements, ranked by atomic number from helium (2) up to zinc (30). When elements up to iron (26) are fused with a helium nucleus (alpha particle) or a deuterium, they release energy, and this energy helps the star continue with more fusion reactions. The isotopes of cobalt (27), nickel (28), copper (29), and zinc (30) produced by fusion are not stable and decay back into lighter elements. Iron-56 (atomic number 26) is the heaviest stable isotope produced by exothermic fusion and subsequent decay.

Our sun produces mostly helium by fusion, but it also uses fusion to make lithium, beryllium and boron. Temperature and mass determine how far a star can go with fusion. Our sun has a core temperature less than 16 million degrees Kelvin. In a star where fusion results in iron, the core temperature has to be over 2.5 billion degrees Kelvin, and this only happens in the final hours or days of the massive star's life, which then ends in a type II supernova. Half the elements with atomic numbers higher than iron are produced during the days- or months- long explosion, but it's not nuclear fusion doing it (which is exothermic), but rather processes known as nuetron capture or proton capture(which are endothermic).

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