Editing Deuterium (section)

=== Big Bang nucleosynthesis ===
{{Main|Big Bang nucleosynthesis}}
Synthesis during the formation of the universe is the only significant way naturally occurring deuterium has been created; it is destroyed in [[stellar fusion]]. Deuterium is thought to have played an important role in setting the number and ratios of the elements that were formed in the [[Big Bang]].<ref>{{Cite journal |last=Particle Data Group |last2=Workman |first2=R L |last3=Burkert |first3=V D |last4=Crede |first4=V |last5=Klempt |first5=E |last6=Thoma |first6=U |last7=Tiator |first7=L |last8=Agashe |first8=K |last9=Aielli |first9=G |last10=Allanach |first10=B C |last11=Amsler |first11=C |last12=Antonelli |first12=M |last13=Aschenauer |first13=E C |last14=Asner |first14=D M |last15=Baer |first15=H |date=2022-08-08 |title=Review of Particle Physics |url=https://academic.oup.com/ptep/article/doi/10.1093/ptep/ptac097/6651666 |journal=Progress of Theoretical and Experimental Physics |language=en |volume=2022 |issue=8 |doi=10.1093/ptep/ptac097 |issn=2050-3911|hdl=1854/LU-01HQG4F6CV7P2F3WWNH4RRN8HD |hdl-access=free }}</ref>{{rp|loc=24.2}} Combining [[thermodynamics]] and the changes brought about by cosmic expansion, one can calculate the fraction of [[protons]] and [[neutrons]] based on the temperature at the point that the universe cooled enough to allow formation of [[Atomic nucleus|nuclei]]. This calculation indicates seven protons for every neutron at the beginning of [[nucleogenesis]], a ratio that would remain stable even after nucleogenesis was over. This fraction was in favor of protons initially, primarily because the lower mass of the proton favored their production. As the Universe expanded, it cooled. [[Free neutron]]s and protons are less stable than [[helium]] nuclei, and the protons and neutrons had a strong energetic reason to form [[helium-4]]. However, forming helium-4 requires the intermediate step of forming deuterium.

Through much of the few minutes after the Big Bang during which nucleosynthesis could have occurred, the temperature was high enough that the mean energy per particle was greater than the binding energy of weakly bound deuterium; therefore, any deuterium that was formed was immediately destroyed. This situation is known as the '''deuterium bottleneck'''. The bottleneck delayed formation of any helium-4 until the Universe became cool enough to form deuterium (at about a temperature equivalent to 100&nbsp;[[keV]]). At this point, there was a sudden burst of element formation (first deuterium, which immediately fused into helium). However, very soon thereafter, at twenty minutes after the Big Bang, the Universe became too cool for any further [[nuclear fusion]] or nucleosynthesis. At this point, the elemental abundances were nearly fixed, with the only change as some of the [[radioactive]] products of Big Bang nucleosynthesis (such as [[tritium]]) decay.<ref>{{cite web |last=Weiss |first=Achim |name-list-style=vanc |title=Equilibrium and change: The physics behind Big Bang nucleosynthesis |website=Einstein Online |url=http://www.einstein-online.info/en/spotlights/BBN_phys/index.html |access-date=2007-02-24 |archive-date=8 February 2007 |archive-url=https://web.archive.org/web/20070208212219/http://www.einstein-online.info/en/spotlights/BBN_phys/index.html |url-status=dead }}</ref> The deuterium bottleneck in the formation of helium, together with the lack of stable ways for helium to combine with hydrogen or with itself (no stable nucleus has a mass number of 5 or 8) meant that an insignificant amount of carbon, or any elements heavier than carbon, formed in the Big Bang. These elements thus required formation in stars. At the same time, the failure of much nucleogenesis during the Big Bang ensured that there would be plenty of hydrogen in the later universe available to form long-lived stars, such as the Sun.