Isotopes of argon: Difference between revisions

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{{Infobox argon isotopes}}
{{Infobox argon isotopes}}
{{Use dmy dates |date=July 2020}}
{{Use dmy dates |date=July 2020}}
[[Argon]] ({{sub|18}}Ar) has 26 known [[isotope]]s, from {{sup|29}}Ar to {{sup|54}}Ar, of which three are [[stable isotope|stable]] ({{sup|36}}Ar, {{sup|38}}Ar, and {{sup|40}}Ar). On Earth, {{sup|40}}Ar makes up 99.6% of natural argon. The longest-lived radioactive isotopes are {{sup|39}}Ar with a half-life of 268 years, {{sup|42}}Ar with a half-life of 32.9 years, and {{sup|37}}Ar with a half-life of 35.04 days. All other isotopes have half-lives of less than two hours, and most less than one minute.
[[Argon]] ({{sub|18}}Ar) has 26 known [[isotope]]s, from {{sup|29}}Ar to {{sup|54}}Ar, of which three are [[stable isotope|stable]] ({{sup|36}}Ar, {{sup|38}}Ar, and {{sup|40}}Ar). On Earth, {{sup|40}}Ar makes up 99.6% of natural argon. The longest-lived radioactive isotopes are {{sup|39}}Ar with a half-life of 268 years, {{sup|42}}Ar with a half-life of 32.9 years, and {{sup|37}}Ar with a half-life of 35.04 days. All other isotopes have half-lives of less than two hours, and most less than one minute. Isotopes lighter than <sup>38</sup>Ar decay to [[chlorine]] or lighter elements, while heavier ones beta decay to [[potassium]].


The naturally occurring [[Potassium-40|{{sup|40}}K]], with a [[half-life]] of 1.248{{x10^|9}} years, decays to stable {{sup|40}}Ar by [[electron capture]] (10.72%) and by [[positron emission]] (0.001%), and also to stable {{sup|40}}Ca via [[beta decay]] (89.28%). These properties and ratios are used to determine the age of [[rock (geology)|rocks]] through [[potassium–argon dating]].<ref name="iso">
The naturally occurring [[Potassium-40|{{sup|40}}K]], with a [[half-life]] of 1.248{{x10^|9}} years, decays to stable {{sup|40}}Ar by [[electron capture]] (10.72%) and by [[positron emission]] (0.001%), and also to stable {{sup|40}}Ca via [[beta decay]] (89.28%). These properties and ratios are used to determine the age of [[rock (geology)|rocks]] through [[potassium–argon dating]].<ref name="iso">
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}}</ref>
}}</ref>


Despite the trapping of {{sup|40}}Ar in many rocks, it can be released by melting, grinding, and diffusion. Almost all argon in the Earth's atmosphere is the product of {{sup|40}}K decay, since 99.6% of Earth's atmospheric argon is {{sup|40}}Ar, whereas in the Sun and presumably in primordial star-forming clouds, argon consists of < 15% {{sup|38}}Ar and mostly (85%) {{sup|36}}Ar. <!--taken from the argon article--> Similarly, the ratio of the isotopes {{sup|36}}Ar:{{sup|38}}Ar:{{sup|40}}Ar in the atmospheres of the [[outer planet]]s is measured to be 8400:1600:1.<ref name="36Ar-Cameron">{{cite journal |last1=Cameron |first1=A.G.W. |author-link1=Alastair G. W. Cameron |title=Elemental and isotopic abundances of the volatile elements in the outer planets |journal=Space Science Reviews |date=1973 |volume=14 |issue=3–4 |pages=392–400 |bibcode=1973SSRv...14..392C |doi=10.1007/BF00214750 |s2cid=119861943}}</ref>
Despite the trapping of {{sup|40}}Ar in many rocks, it can be released by melting, grinding, and diffusion. Almost all argon in the Earth's atmosphere is the product of {{sup|40}}K decay, since 99.6% of Earth's atmospheric argon is {{sup|40}}Ar, whereas in the Sun and presumably in primordial star-forming clouds, argon consists of ~85% {{sup|36}}Ar, ~15% {{sup|38}}Ar and only trace {{sup|40}}Ar. <!--taken from the argon article--> Similarly, the ratio of the isotopes {{sup|36}}Ar:{{sup|38}}Ar:{{sup|40}}Ar in the atmospheres of the [[outer planet]]s is measured to be 8400:1600:1.<ref name="36Ar-Cameron">{{cite journal |last1=Cameron |first1=A.G.W. |author-link1=Alastair G. W. Cameron |title=Elemental and isotopic abundances of the volatile elements in the outer planets |journal=Space Science Reviews |date=1973 |volume=14 |issue=3–4 |pages=392–400 |bibcode=1973SSRv...14..392C |doi=10.1007/BF00214750 |s2cid=119861943}}</ref>


In the Earth's [[atmosphere]], radioactive {{sup|39}}Ar (half-life 268(8) years) is made by [[cosmic ray]] activity, primarily from {{sup|40}}Ar. In the subsurface environment, it is also produced through [[neutron capture]] by {{sup|39}}>K or [[alpha decay|alpha emission]] by [[calcium]]. The content of {{sup|39}}Ar in natural argon is measured to be of (8.0±0.6)×10{{sup|−16}} g/g, or (1.01±0.08)&nbsp;Bq/kg of {{sup|36, 38, 40}}Ar.<ref name="40Ar-Benetti">
In the Earth's [[atmosphere]], radioactive {{sup|39}}Ar (and to a lesser extent <sup>37</sup>Ar) is made by [[cosmic ray]] activity, primarily from {{sup|40}}Ar. In the subsurface environment, {{sup|39}}Ar is also produced through [[neutron capture]] by {{sup|39}}K or <sup>42</sup>Ca, with proton or alpha emission respectively; <sup>37</sup>Ar was created in subsurface [[nuclear testing|nuclear explosions]] similarly from <sup>40</sup>Ca.<ref name="iso"/> The content of {{sup|39}}Ar in natural argon is measured to be of (8.0±0.6)×10{{sup|−16}} g/g, or (1.01±0.08)&nbsp;Bq/kg weight.<ref name="40Ar-Benetti">
{{cite journal  
{{cite journal  
|author=P. Benetti
|author=P. Benetti
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|doi=10.1016/j.nima.2007.01.106
|doi=10.1016/j.nima.2007.01.106
|s2cid=17073444
|s2cid=17073444
}}</ref> The content of <sup>42</sup>Ar (half-life 33 years) in the Earth's atmosphere is lower than 6×10<sup>−21</sup> parts per part of <sup>36, 38, 40</sup>Ar.<ref name="40Ar-Ashitkov">
}}</ref> The content of <sup>42</sup>Ar (half-life 33 years) in the Earth's atmosphere, though it had previously been reported as a cosmogenic isotope,<ref>For example in {{cite journal |last1=Barabash |first1=A.S. |last2=Saakyan |first2=R.R. |last3=Umatov |first3=V.I. |year=2016 |title=On concentration of 42Ar in the Earth's atmosphere |journal=Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment |doi=10.1016/j.nima.2016.09.042|arxiv=1609.08890 }}</ref> is lower than 6×10<sup>−21</sup> of the element.<ref name="40Ar-Ashitkov">
{{cite journal
{{cite journal
|author=V. D. Ashitkov
|author=V. D. Ashitkov
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|volume=37 |pages=1105–1112
|volume=37 |pages=1105–1112
|display-authors=etal |bibcode=2012PhPro..37.1105B
|display-authors=etal |bibcode=2012PhPro..37.1105B
|doi=10.1016/j.phpro.2012.04.099 |doi-access=free}}</ref> Lighter radioactive isotopes can decay to different elements (usually [[chlorine]]) while heavier ones decay to [[potassium]].
|doi=10.1016/j.phpro.2012.04.099 |doi-access=free}}</ref>


<sup>36</sup>Ar, in the form of [[argon hydride]], was detected in the [[Crab Nebula]] [[supernova remnant]] during 2013.<ref name="NYT-20131213">{{cite news |last=Quenqua |first=Douglas |title=Noble Molecules Found in Space |date=13 December 2013 |work=[[The New York Times]] |url=https://www.nytimes.com/2013/12/17/science/space/noble-molecules-found-in-space.html |access-date=13 December 2013}}</ref><ref name="SCI-2013">
<sup>36</sup>Ar, in the form of [[argon hydride]], was detected in the [[Crab Nebula]] [[supernova remnant]] during 2013.<ref name="NYT-20131213">{{cite news |last=Quenqua |first=Douglas |title=Noble Molecules Found in Space |date=13 December 2013 |work=[[The New York Times]] |url=https://www.nytimes.com/2013/12/17/science/space/noble-molecules-found-in-space.html |access-date=13 December 2013}}</ref><ref name="SCI-2013">
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|s2cid=37578581
|s2cid=37578581
}}</ref> This was the first time a [[noble gas compound|noble molecule]] was detected in [[outer space]].<ref name="NYT-20131213"/><ref name="SCI-2013"/>
}}</ref> This was the first time a [[noble gas compound|noble molecule]] was detected in [[outer space]].<ref name="NYT-20131213"/><ref name="SCI-2013"/>
<sup>37</sup>Ar is a synthetic radionuclide that is created via [[neutron capture]] of <sup>40</sup>Ca followed by [[alpha particle]] emission, as a result of subsurface [[nuclear testing|nuclear explosions]]. It has a half-life of 35 days.<ref name="iso"/>


==List of isotopes==
==List of isotopes==

Latest revision as of 06:15, 28 June 2025

Template:Short description Template:Infobox argon isotopes Template:Use dmy dates Argon (18Ar) has 26 known isotopes, from 29Ar to 54Ar, of which three are stable (36Ar, 38Ar, and 40Ar). On Earth, 40Ar makes up 99.6% of natural argon. The longest-lived radioactive isotopes are 39Ar with a half-life of 268 years, 42Ar with a half-life of 32.9 years, and 37Ar with a half-life of 35.04 days. All other isotopes have half-lives of less than two hours, and most less than one minute. Isotopes lighter than 38Ar decay to chlorine or lighter elements, while heavier ones beta decay to potassium.

The naturally occurring 40K, with a half-life of 1.248×10Template:Val years, decays to stable 40Ar by electron capture (10.72%) and by positron emission (0.001%), and also to stable 40Ca via beta decay (89.28%). These properties and ratios are used to determine the age of rocks through potassium–argon dating.[1]

Despite the trapping of 40Ar in many rocks, it can be released by melting, grinding, and diffusion. Almost all argon in the Earth's atmosphere is the product of 40K decay, since 99.6% of Earth's atmospheric argon is 40Ar, whereas in the Sun and presumably in primordial star-forming clouds, argon consists of ~85% 36Ar, ~15% 38Ar and only trace 40Ar. Similarly, the ratio of the isotopes 36Ar:38Ar:40Ar in the atmospheres of the outer planets is measured to be 8400:1600:1.[2]

In the Earth's atmosphere, radioactive 39Ar (and to a lesser extent 37Ar) is made by cosmic ray activity, primarily from 40Ar. In the subsurface environment, 39Ar is also produced through neutron capture by 39K or 42Ca, with proton or alpha emission respectively; 37Ar was created in subsurface nuclear explosions similarly from 40Ca.[1] The content of 39Ar in natural argon is measured to be of (8.0±0.6)×10−16 g/g, or (1.01±0.08) Bq/kg weight.[3] The content of 42Ar (half-life 33 years) in the Earth's atmosphere, though it had previously been reported as a cosmogenic isotope,[4] is lower than 6×10−21 of the element.[5] Many endeavors require argon depleted in the cosmogenic isotopes, known as depleted argon.[6]

36Ar, in the form of argon hydride, was detected in the Crab Nebula supernova remnant during 2013.[7][8] This was the first time a noble molecule was detected in outer space.[7][8]

List of isotopes

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Template:Isotopes table |-id=Argon-29 | 29Ar[9] | style="text-align:right" | 18 | style="text-align:right" | 11 | 29.04076(47)# | | 2p | 27S | 5/2+# | | |-id=Argon-30 | 30Ar | style="text-align:right" | 18 | style="text-align:right" | 12 | 30.02369(19)# | <10 ps | 2p | 28S | 0+ | | |-id=Argon-31 | rowspan=7|31Ar | rowspan=7 style="text-align:right" | 18 | rowspan=7 style="text-align:right" | 13 | rowspan=7|31.01216(22)# | rowspan=7|15.0(3) ms | β+, p (68.3%) | 30S | rowspan=7|5/2+ | rowspan=7| | rowspan=7| |- | β+ (22.63%) | 31Cl |- | β+, 2p (9.0%) | 29P |- | β+, 3p (0.07%) | 28Si |- | β+, p, α? (<0.38%) | 26Si |- | β+, α? (<0.03%) | 27P |- | 2p? (<0.03%) | 29S |-id=Argon-32 | rowspan=2|32Ar | rowspan=2 style="text-align:right" | 18 | rowspan=2 style="text-align:right" | 14 | rowspan=2|31.9976378(19) | rowspan=2|98(2) ms | β+ (64.42%) | 32Cl | rowspan=2|0+ | rowspan=2| | rowspan=2| |- | β+, p (35.58%) | 31S |-id=Argon-33 | rowspan=2|33Ar | rowspan=2 style="text-align:right" | 18 | rowspan=2 style="text-align:right" | 15 | rowspan=2|32.98992555(43) | rowspan=2|173.0(20) ms | β+ (61.3%) | 33Cl | rowspan=2|1/2+ | rowspan=2| | rowspan=2| |- | β+, p (38.7%) | 32S |-id=Argon-34 | 34Ar | style="text-align:right" | 18 | style="text-align:right" | 16 | 33.980270092(83) | 846.46(35) ms | β+ | 34Cl | 0+ | | |-id=Argon-35 | 35Ar | style="text-align:right" | 18 | style="text-align:right" | 17 | 34.97525772(73) | 1.7756(10) s | β+ | 35Cl | 3/2+ | | |-id=Argon-36 | 36Ar | style="text-align:right" | 18 | style="text-align:right" | 18 | 35.967545106(28) | colspan=3 align=center|Observationally Stable[n 1] | 0+ | 0.003336(210) | |-id=Argon-37 | 37Ar | style="text-align:right" | 18 | style="text-align:right" | 19 | 36.96677630(22) | 35.011(19) d | EC | 37Cl | 3/2+ | Trace[n 2] | |-id=Argon-38 | 38Ar | style="text-align:right" | 18 | style="text-align:right" | 20 | 37.96273210(21) | colspan=3 align=center|Stable | 0+ | 0.000629(70) | |-id=Argon-39 | 39Ar[n 3] | style="text-align:right" | 18 | style="text-align:right" | 21 | 38.9643130(54) | Template:Val y[10] | β− | 39K | 7/2− | Template:Val[11][n 2] | |-id=Argon-40 | 40Ar[n 4] | style="text-align:right" | 18 | style="text-align:right" | 22 | 39.9623831220(23) | colspan=3 align=center|Stable | 0+ | 0.996035(250)[n 5] | |-id=Argon-41 | 41Ar | style="text-align:right" | 18 | style="text-align:right" | 23 | 40.96450057(37) | 109.61(4) min | β− | 41K | 7/2− | Trace[n 2] | |-id=Argon-42 | 42Ar | style="text-align:right" | 18 | style="text-align:right" | 24 | 41.9630457(62) | 32.9(11) y | β− | 42K | 0+ | | |-id=Argon-43 | 43Ar | style="text-align:right" | 18 | style="text-align:right" | 25 | 42.9656361(57) | 5.37(6) min | β− | 43K | 5/2(−) | | |-id=Argon-44 | 44Ar | style="text-align:right" | 18 | style="text-align:right" | 26 | 43.9649238(17) | 11.87(5) min | β− | 44K | 0+ | | |-id=Argon-45 | 45Ar | style="text-align:right" | 18 | style="text-align:right" | 27 | 44.96803973(55) | 21.48(15) s | β− | 45K | (5/2−,7/2−) | | |-id=Argon-46 | 46Ar | style="text-align:right" | 18 | style="text-align:right" | 28 | 45.9680392(25) | 8.4(6) s | β− | 46K | 0+ | | |-id=Argon-47 | rowspan=2|47Ar | rowspan=2 style="text-align:right" | 18 | rowspan=2 style="text-align:right" | 29 | rowspan=2|46.9727671(13) | rowspan=2|1.23(3) s | β− (>99.8%) | 47K | rowspan=2|(3/2)− | rowspan=2| | rowspan=2| |- | β−, n? (<0.2%) | 46K |-id=Argon-48 | rowspan=2|48Ar | rowspan=2 style="text-align:right" | 18 | rowspan=2 style="text-align:right" | 30 | rowspan=2|47.976001(18) | rowspan=2|415(15) ms | β− (62%) | 48K | rowspan=2|0+ | rowspan=2| | rowspan=2| |- | β−, n (38%) | 47K |-id=Argon-49 | rowspan=3|49Ar | rowspan=3 style="text-align:right" | 18 | rowspan=3 style="text-align:right" | 31 | rowspan=3|48.98169(43)# | rowspan=3|236(8) ms | β− | 49K | rowspan=3|3/2−# | rowspan=3| | rowspan=3| |- | β−, n (29%) | 48K |- | β−, 2n? | 47K |-id=Argon-50 | rowspan=3|50Ar | rowspan=3 style="text-align:right" | 18 | rowspan=3 style="text-align:right" | 32 | rowspan=3|49.98580(54)# | rowspan=3|106(6) ms | β− (63%) | 50K | rowspan=3|0+ | rowspan=3| | rowspan=3| |- | β−, n (37%) | 49K |- | β−, 2n? | 48K |-id=Argon-51 | rowspan=3|51Ar | rowspan=3 style="text-align:right" | 18 | rowspan=3 style="text-align:right" | 33 | rowspan=3|50.99303(43)# | rowspan=3|30# ms
[>200 ns] | β−? | 51K | rowspan=3|1/2−# | rowspan=3| | rowspan=3| |- | β−, n? | 50K |- | β−, 2n? | 49K |-id=Argon-52 | rowspan=3|52Ar | rowspan=3 style="text-align:right" | 18 | rowspan=3 style="text-align:right" | 34 | rowspan=3|51.99852(64)# | rowspan=3|40# ms
[>620 ns] | β−? | 52K | rowspan=3|0+ | rowspan=3| | rowspan=3| |- | β−, n? | 51K |- | β−, 2n? | 50K |-id=Argon-53 | rowspan=3|53Ar | rowspan=3 style="text-align:right" | 18 | rowspan=3 style="text-align:right" | 35 | rowspan=3|53.00729(75)# | rowspan=3|20# ms
[>620 ns] | β−? | 53K | rowspan=3|5/2−# | rowspan=3| | rowspan=3| |- | β−, n? | 52K |- | β−, 2n? | 51K |-id=Argon-54 | rowspan=3|54Ar | rowspan=3 style="text-align:right" | 18 | rowspan=3 style="text-align:right" | 36 | rowspan=3|54.01348(86)# | rowspan=3|5# ms
[>400 ns] | β−? | 54K | rowspan=3|0+ | rowspan=3| | rowspan=3| |- | β−, n? | 53K |- | β−, 2n? | 52K Template:Isotopes table/footer

See also

Daughter products other than argon

References

Template:Reflist

External links

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