Editing Big Bang nucleosynthesis (section)

==History==
The history of Big Bang nucleosynthesis research began with a proposal<ref>{{Cite journal |last=Gamow |first=G. |date=1948-08-15 |title=The Origin of Elements and the Separation of Galaxies |url=https://journals.aps.org/pr/abstract/10.1103/PhysRev.74.505.2 |journal=Physical Review |volume=74 |issue=4 |pages=505–506 |doi=10.1103/PhysRev.74.505.2}}</ref><ref>{{Cite journal |last=Gamow |first=G. |date=October 1948 |title=The Evolution of the Universe |url=https://www.nature.com/articles/162680a0 |journal=Nature |language=en |volume=162 |issue=4122 |pages=680–682 |doi=10.1038/162680a0 |issn=0028-0836}}</ref> in the 1940s by [[George Gamow]] that nuclear reactions during a hot initial phase of the universe produced the observed hydrogen and helium. Calculations by his student [[Ralph Alpher]] were published<ref>{{cite journal|last1=Alpher|first1=R. A.|last2=Bethe|first2=H.|author-link2=Hans Bethe|last3=Gamow|first3=G.|author-link3=George Gamow|date=1 April 1948|title=The Origin of Chemical Elements|journal=[[Physical Review]]|volume=73|issue=7|pages=803–804|bibcode=1948PhRv...73..803A|doi=10.1103/PhysRev.73.803|pmid=18877094|author-link1=Ralph Asher Alpher|doi-access=free}}<!--|access-date=2011-03-10 --></ref> in the famous [[Alpher–Bethe–Gamow paper]] outlined a theory of light-element production in the early universe. The first detailed calculations of the primordial isotopic abundances came in 1966<ref name="Primordial Helium">{{Cite journal | doi=10.1103/PhysRevLett.16.410| title=Primeval Helium Abundance and the Primeval Fireball| journal=Physical Review Letters| volume=16| issue=10| pages=410–413| year=1966| last1=Peebles| first1=P. J. E.| bibcode=1966PhRvL..16..410P}}</ref><ref name="Primordial Elements">Wagoner, Fowler and Hoyle [http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1967ApJ...148....3W&amp;data_type=PDF_HIGH&amp;whole_paper=YES&amp;type=PRINTER&amp;filetype=.pdf "ON THE SYNTHESIS OF ELEMENTS AT VERY HIGH TEMPERATURES"], ''Robert V. Wagoner, William A. Fowler, and F. Hoyle, The Astrophysical Journal, Vol. 148, April 1967.''</ref>  and have been refined over the years using updated estimates of the input nuclear reaction rates.<ref>{{Cite book |last=Hashimoto |first=Masa-aki |url=https://link.springer.com/book/10.1007/978-981-13-2935-7 |title=Big-Bang Nucleosynthesis: Thermonuclear History in the Early Universe |last2=Nakamura |first2=Riou |last3=Thushari |first3=E. P. Berni Ann |last4=Arai |first4=Kenzo |date=2018 |publisher=Springer |isbn=978-981-13-2935-7 |series=SpringerBriefs in Physics Ser |location=Singapore |language=en |doi=10.1007/978-981-13-2935-7 |issn=2191-5423}}</ref>{{rp|3}} The first systematic [[Monte Carlo integration|Monte Carlo]] study of how nuclear reaction rate uncertainties impact isotope predictions, over the relevant temperature range, was carried out in 1993.<ref name="Primordial Elements Monte Carlo">Smith, Kawano, and Malaney. [http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1993ApJS...85..219S&amp;data_type=PDF_HIGH&amp;whole_paper=YES&amp;type=PRINTER&amp;filetype=.pdf "EXPERIMENTAL, COMPUTATIONAL, AND OBSERVATIONAL ANALYSIS OF PRIMORDIAL NUCLEOSYNTHESIS"], ''Michael S. Smith, Lawrence H. Kawano and Robert A. Malaney, The Astrophysical Journal Supplement Series, 85:219-247, 1993 April.''</ref>