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Big Bang nucleosynthesis
Physical cosmology Universe · Big Bang Age of the universe Timeline of the Big Bang Ultimate fate of the universe Inflation · Nucleosynthesis GWB · Neutrino background Cosmic microwave background Redshift · Hubble's law Metric expansion of space Friedmann equations FLRW metric Shape of the universe Structure formation Reionization Galaxy formation Large-scale structure Galaxy filament Lambda-CDM model Dark energy · Dark matter Dark fluid · Dark flow Timeline of cosmological theories Future of an expanding universe Observational cosmology 2dF · SDSS COBE · BOOMERanG · WMAP · Planck v d e In physical cosmology, Big Bang nucleosynthesis (or primordial nucleosynthesis, abbreviated BBN) refers to the production of nuclei other than those of H-1 (i.e. the normal, light isotope of hydrogen, whose nuclei consist of a single proton each) during the early phases of the universe. Primordial nucleosynthesis took place just a few moments after the Big Bang and is believed to be responsible for the formation of a heavier isotope of hydrogen known as deuterium (H-2 or D), the helium isotopes He-3 and He-4, and the lithium isotopes Li-6 and Li-7. In addition to these stable nuclei some unstable, or radioactive, isotopes were also produced during primordial nucleosynthesis: tritium or H-3; beryllium-7 (Be-7), and beryllium-8 (Be-8). These unstable isotopes either decayed or fused with other nuclei to make one of the stable isotopes.
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