Editing Natural abundance

{{short description|Relative proportion of an isotope as found in nature}}
{{Use dmy dates|date=March 2018}}
[[File:Relative_abundance_of_elements.png | thumb | right | Relative abundance of elements in the Earth's upper crust]]
In [[physics]], '''natural abundance''' (NA) refers to the abundance of [[isotope]]s of a [[chemical element]] as naturally found on a [[planet]]. The relative atomic mass (a weighted average, weighted by [[mole fraction|mole-fraction]] abundance figures) of these isotopes is the [[atomic weight]] listed for the element in the [[periodic table]]. The abundance of an isotope varies from planet to planet, and even from place to place on the Earth, but remains relatively constant in time (on a short-term scale).

As an example, [[uranium]] has [[isotopes of uranium|three naturally occurring isotopes]]: <sup>238</sup>U, <sup>235</sup>U, and <sup>234</sup>U. Their respective natural mole-fraction abundances are 99.2739–99.2752%, 0.7198–0.7202%, and 0.0050–0.0059%.<ref>{{cite web |work=[[GlobalSecurity.org]] |title=Uranium Isotopes |url=https://www.globalsecurity.org/wmd/intro/u-isotopes.htm |access-date=14 March 2012}}</ref> For example, if 100,000 uranium atoms were analyzed, one would expect to find approximately 99,274 <sup>238</sup>U atoms, approximately 720 <sup>235</sup>U atoms, and very few (most likely 5 or 6) <sup>234</sup>U atoms. This is because <sup>238</sup>U is much more stable than <sup>235</sup>U or <sup>234</sup>U, as the [[half-life]] of each isotope reveals: 4.468&nbsp;×&nbsp;10<sup>9</sup> years for <sup>238</sup>U compared with 7.038&nbsp;×&nbsp;10<sup>8</sup> years for <sup>235</sup>U and 245,500 years for <sup>234</sup>U.

Exactly because the different uranium isotopes have different half-lives, when the Earth was younger, the isotopic composition of uranium was different. As an example, 1.7×10<sup>9</sup> years ago the NA of <sup>235</sup>U was 3.1% compared with today's 0.7%, and that allowed a [[natural nuclear fission reactor]] to form, something that cannot happen today.

However, the natural abundance of a given isotope is also affected by the probability of its creation in [[nucleosynthesis]] (as in the case of [[samarium]]; radioactive [[samarium-147|<sup>147</sup>Sm]] and <sup>148</sup>Sm are much more abundant than stable <sup>144</sup>Sm) and by production of a given isotope as a daughter of natural radioactive isotopes (as in the case of radiogenic [[isotopes of lead]]).

==Deviations from natural abundance==
It is now known from study of the Sun and primitive meteorites that the [[Solar System]] was initially almost homogeneous in isotopic composition. Deviations from the (evolving) galactic average, locally sampled around the time that the Sun's nuclear burning began, can generally be accounted for by mass fractionation (see the article on [[mass-independent fractionation]]) plus a limited number of nuclear decay and transmutation processes.<ref>{{cite journal |first=Robert N. |last=Clayton |date=1978 |title=Isotopic anomalies in the early solar system |journal=[[Annual Review of Nuclear and Particle Science]] |volume=28 |pages=501–522 |doi=10.1146/annurev.ns.28.120178.002441 |doi-access= |bibcode=1978ARNPS..28..501C}}</ref> There is also evidence for injection of short-lived (now-extinct) isotopes from a nearby supernova explosion that may have triggered solar nebula collapse.<ref>{{cite journal |last=Zinner |first=Ernst |title=An isotopic view of the early solar system |journal=Science |date=2003 |volume=300 |issue=5617 |pages=265–267 |doi=10.1126/science.1080300 |pmid=12690180 |s2cid=118638578 |url=https://www.science.org/doi/abs/10.1126/science.1080300|url-access=subscription }}</ref> Hence deviations from natural abundance on Earth are often measured in parts per thousand ([[per mille]] or ‰) because they are less than one percent (%).

An exception to this lies with the [[presolar grains]] found in primitive meteorites. These small grains condensed in the outflows of evolved ("dying") stars and escaped the mixing and homogenization processes in the interstellar medium and the solar accretion disk (also known as the solar nebula or protoplanetary disk).<ref name=anders/>{{clarify|This homogenization process at the stellar-disk level has not been described in the article|date=October 2019}} As stellar condensates ("stardust"), these grains carry the isotopic signatures of specific nucleosynthesis processes in which their elements were made.<ref>{{cite journal |first=Ernst |last=Zinner |date=1998 |title=Stellar nucleosynthesis and the isotopic composition of presolar grains from primitive meteorites |journal=[[Annual Review of Earth and Planetary Sciences]] |volume=26 |pages=147–188 |doi=10.1146/annurev.earth.26.1.147 |bibcode=1998AREPS..26..147Z}}</ref> In these materials, deviations from "natural abundance" are sometimes measured in factors of 100.{{citation needed|date=October 2019}}<ref name=anders>{{cite journal |last1=Anders |first1=Edward |last2=Zinner |first2=Ernst |title=Interstellar Grains in Primitive Meteorites: Diamond, Silicon Carbide, and Graphite |journal=Meteoritics |year=1993 |volume=28 |issue=4 |pages=490–514 |bibcode=1993Metic..28..490A |doi=10.1111/j.1945-5100.1993.tb00274.x |url=https://onlinelibrary.wiley.com/doi/abs/10.1111/j.1945-5100.1993.tb00274.x|url-access=subscription }}</ref>

==Natural isotope abundance of some elements==
The next table gives the [[Earth|terrestrial]]<!-- needs the qualifying adjective, as the source supports only distributions on Earth --> isotope distributions for some elements. Some elements, such as [[phosphorus]] and [[fluorine]], only exist as a single isotope, with a natural abundance of 100%.

{| class="wikitable"
|+Natural isotope abundance of some elements on Earth<ref>{{RubberBible83rd}}</ref>
|-
! ''Isotope'' || % nat. abundance !! atomic mass
|-
| {{sup|1}}H || 99.985 || 1.007825
|-
| [[Deuterium|{{sup|2}}H]] || 0.015 || 2.0140
|-
| [[Carbon-12|{{sup|12}}C]] || 98.89 || 12 (formerly by definition)
|-
| [[Carbon-13|{{sup|13}}C]] || 1.11 || 13.00335
|-
| {{sup|14}}N || 99.64 || 14.00307
|-
| {{sup|15}}N || 0.36 || 15.00011
|-
| [[Oxygen-16|{{sup|16}}O]] || 99.76 || 15.99491
|-
| [[Oxygen-17|{{sup|17}}O]] || 0.04|| 16.99913
|-
| [[Oxygen-18|{{sup|18}}O]] || 0.2|| 17.99916
|-
| {{sup|28}}Si || 92.23 || 27.97693
|-
| {{sup|29}}Si || 4.67 || 28.97649
|-
| {{sup|30}}Si || 3.10 || 29.97376
|-
| {{sup|32}}S || 95.0 || 31.97207
|-
| {{sup|33}}S || 0.76 || 32.97146
|-
| {{sup|34}}S || 4.22 || 33.96786
|-
| {{sup|35}}Cl || 75.77 || 34.96885
|-
| {{sup|37}}Cl || 24.23 || 36.96590
|-
| {{sup|79}}Br || 50.69 || 78.9183
|-
| {{sup|81}}Br || 49.31 || 80.9163
|}

==See also==
* [[Abundance of the chemical elements]]
* [[Decay product]]
* [[Isotope]]
* [[Presolar grains]]
* [[Radionuclide]]

==References==
{{Reflist}}

==External links==
* [https://web.archive.org/web/20150707182753/http://ie.lbl.gov/education/isotopes.htm Berkeley Isotopes Project Interactive Table] (archived 2015)
* [https://www.sisweb.com/referenc/source/exactmas.htm Exact Masses of the Elements and Isotopic Abundances], Scientific Instrument Services
* [https://web.archive.org/web/20110826012824/http://research.smilems.com/molecule-tk/ Tools to compute low- and high-precision isotopic distribution] (archived 2011)

{{Chemical solutions}}

[[Category:Chemical properties]]
[[Category:Isotopes]]