Supernova nucleosynthesis

Supernova nucleosynthesis is the production of atomic nuclei during stellar explosions. Explosive reactions create or alter elements, which are then dispersed into space by the ejecta.

Explosive silicon burning: High-temperature fusion reactions that rearrange silicon-group nuclei into iron-group elements during a supernova. It produces much of the iron-group material in ejecta heated by the shock.
Stellar nucleosynthesis: The production of chemical elements by nuclear reactions inside stars and during their evolution. Supernova nucleosynthesis extends element production beyond the star's pre-explosion burning stages.
B2FH paper: A 1957 review by Burbidge, Burbidge, Fowler, and Hoyle that organized major mechanisms of stellar element synthesis. It established a framework for assigning cosmic abundances to stellar processes.
Galactic chemical evolution: The changes in a galaxy's chemical composition over time through stellar production, gas flows, and star formation. Supernova yields enrich interstellar gas from which later generations of stars form.
R-process site: The astrophysical environment or environments in which rapid neutron capture produces heavy nuclei. Whether ordinary supernovae contribute substantially remains disputed alongside compact-object mergers.
Rapid neutron-capture process: A nucleosynthesis process in which nuclei capture neutrons faster than they can undergo beta decay. Neutron-rich supernova ejecta have been proposed as a site for this process.
Neutron capture: A nuclear reaction in which an atomic nucleus absorbs a free neutron. Capturing neutrons builds heavier nuclei when explosive ejecta provide a suitable neutron supply.
Geoffrey Burbidge: An English-born astronomer who studied stellar nucleosynthesis and coauthored the influential B2FH paper. His work helped articulate how stellar explosions contribute to element formation.
Cosmic-ray nucleosynthesis: The production of some light nuclei when energetic cosmic rays collide with interstellar matter. It offers a distinct origin for light elements that supernova ejecta do not readily explain.
Neutrino-driven wind: A flow of hot matter expelled from a newly formed neutron star by intense neutrino heating. Its neutron richness and expansion history determine whether it can make heavy r-process nuclei.

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