Nucleosynthesis

Nucleosynthesis is the formation of atomic nuclei from protons, neutrons, or lighter nuclei through nuclear reactions. It produces the elements in stars, cosmic explosions, and the early universe.

Stellar nucleosynthesis: The production of nuclei through nuclear reactions inside stars. Fusion in stellar interiors builds many elements up to iron.
B2FH paper: A 1957 review by Margaret Burbidge, Geoffrey Burbidge, William Fowler, and Fred Hoyle on stellar element formation. It established a framework connecting stellar processes to the origins of the elements.
Nuclear fusion: A nuclear reaction in which light nuclei combine to form a heavier nucleus. Fusion powers stars and builds nuclei up to the iron-group region.
Stellar spectroscopy: The study of stars through the wavelengths of their emitted or absorbed light. Spectral lines reveal which elements stellar atmospheres contain.
Neutron star merger: A collision and coalescence of two neutron stars in a binary system. Such mergers provide an observed site for rapid neutron capture, though their total contribution remains under study.
Big Bang nucleosynthesis: The formation of light nuclei during the universe’s first minutes. The early universe’s heat and expansion produced hydrogen, helium, and trace light isotopes.
Geoffrey Burbidge: An astrophysicist who helped develop the theory of stellar element formation. His work with three collaborators synthesized evidence for multiple nucleosynthesis processes.
Neutron capture: A nuclear reaction in which an atomic nucleus absorbs a neutron. Capturing neutrons enables element formation beyond what ordinary stellar fusion can achieve.
Metallicity: In astronomy, the proportion of a star or gas cloud made of elements heavier than helium. Metallicity tracks how much earlier generations of stars enriched cosmic material.
Kilonova: A transient, bright astronomical event powered by radioactive material ejected in a neutron star merger. Its light can carry evidence of freshly synthesized heavy elements.

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