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Remarkably, the Solar neutrinos were discovered by an experiment using a radiochemical method based on chlorine-37 transmutation.<ref name="SciAm">
Remarkably, the Solar neutrinos were discovered by an experiment using a radiochemical method based on chlorine-37 transmutation.<ref name="SciAm">
{{cite journal|doi=10.1038/scientificamerican0769-28|author=J.N. Bahcall|title=Neutrinos from the Sun|url=http://www.sns.ias.edu/~jnb/Papers/Popular/Scientificamerican69/scientificamerican69.html|journal = [[Scientific American]]|volume = 221 |issue = 1 |year = 1969|pages=28–37|bibcode=1969SciAm.221a..28B}}</ref>
{{cite journal
|doi=10.1038/scientificamerican0769-28
|author=J.N. Bahcall
|title=Neutrinos from the Sun
|url=http://www.sns.ias.edu/~jnb/Papers/Popular/Scientificamerican69/scientificamerican69.html
|journal = [[Scientific American]]
|volume = 221 |issue = 1 |year = 1969
|pages=28–37
|bibcode=1969SciAm.221a..28B}}</ref>


==Neutrino detection==
==Neutrino detection==
{{Main|Homestake experiment}}
{{Main|Homestake experiment}}


One of the historically important radiochemical methods of solar [[Neutrino detector|neutrino detection]] is based on inverse [[electron capture]] triggered by the absorption of an [[electron neutrino]].<ref name="Sutton">
One of the historically important radiochemical methods of solar [[Neutrino detector|neutrino detection]] is based on inverse [[electron capture]] triggered by the absorption of an [[electron neutrino]].<ref name="Sutton">
{{cite book|last=Sutton|first=Christine|title=Spaceship Neutrino|url=https://books.google.com/books?id=JBOdejRrmaMC&pg=PA151&lpg=PA151&dq=chlorine-37+neutrino|publisher=[[Cambridge University Press]]|pages=151–152|year=1992|isbn=978-0-521-36404-1|oclc=25246163}}</ref> Chlorine-37 transmutes into Argon-37 via the reaction<ref>
{{cite book
{{cite book|author=F.H. Shu|title=The Physical Universe: An Introduction to Astronomy|url=https://books.google.com/books?id=v_6PbAfapSAC&pg=PA122&lpg=PA122&dq=chlorine+37+neutrino|publisher=University Science Books|page=122|year=1982|isbn=978-0-935702-05-7}}</ref>
|last=Sutton
|first=Christine
|title=Spaceship Neutrino
|url=https://books.google.com/books?id=JBOdejRrmaMC&pg=PA151&lpg=PA151&dq=chlorine-37+neutrino
|publisher=[[Cambridge University Press]]
|pages=151–152
|year=1992
|isbn=978-0-521-36404-1
|oclc=25246163
}}</ref> Chlorine-37 transmutes into Argon-37 via the reaction<ref>
{{cite book
|author=F.H. Shu
|title=The Physical Universe: An Introduction to Astronomy
|url=https://books.google.com/books?id=v_6PbAfapSAC&pg=PA122&lpg=PA122&dq=chlorine+37+neutrino
|publisher=University Science Books
|page=122
|year=1982
|isbn=978-0-935702-05-7
}}</ref>
:{{SimpleNuclide|Chlorine|37}} + {{Subatomic particle|Electron neutrino}} → {{SimpleNuclide|Argon|37}} + {{Subatomic particle|Electron-}}.
:{{SimpleNuclide|Chlorine|37}} + {{Subatomic particle|Electron neutrino}} → {{SimpleNuclide|Argon|37}} + {{Subatomic particle|Electron-}}.


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These last reactions involve [[Auger electron]]s of specific energies.<ref name="Sutton"/><ref>
These last reactions involve [[Auger electron]]s of specific energies.<ref name="Sutton"/><ref>
{{cite journal|author=A.H. Snell, F. Pleasonton|title=Spectrometry of the Neutrino Recoils of Argon-37|journal=[[Physical Review]]|volume=100 |issue=5 |pages=1396–1403|year=1955|doi=10.1103/PhysRev.100.1396
{{cite journal
⚫
|bibcode = 1955PhRv..100.1396S}}</ref> The detection of these electrons confirms that a neutrino event took place. Detection methods involve several hundred thousand liters of [[carbon tetrachloride]] (CCl<sub>4</sub>) or [[tetrachloroethylene]]<!--Also known as perchloroethylene, perchloroethene, perc, PCE --> (C<sub>2</sub>Cl<sub>4</sub>) stored in underground tanks.<ref name="SciAm"/><ref name="Sutton"/><ref>{{cite book|author = A. Bhatnagar, W. Livingston|title = Fundamental of Solar Astronomy|url = https://books.google.com/books?id=fe7XDuxCYjcC&pg=PA88&lpg=PA88&dq=chlorine+37+neutrino|publisher=[[World Scientific]]|pages=87–89|year=2005|isbn=978-981-238-244-3}}</ref>
|author=A.H. Snell, F. Pleasonton
|title=Spectrometry of the Neutrino Recoils of Argon-37
|journal=[[Physical Review]]
|volume=100 |issue=5 |pages=1396–1403
|year=1955
|doi=10.1103/PhysRev.100.1396
⚫
|bibcode = 1955PhRv..100.1396S }}</ref> The detection of these electrons confirms that a neutrino event took place. Detection methods involve several hundred thousand liters of [[carbon tetrachloride]] (CCl<sub>4</sub>) or [[tetrachloroethylene]]<!--Also known as perchloroethylene, perchloroethene, perc, PCE --> (C<sub>2</sub>Cl<sub>4</sub>) stored in underground tanks.<ref name="SciAm"/><ref name="Sutton"/><ref>{{cite book
|author = A. Bhatnagar, W. Livingston
|title = Fundamental of Solar Astronomy
|url = https://books.google.com/books?id=fe7XDuxCYjcC&pg=PA88&lpg=PA88&dq=chlorine+37+neutrino
|publisher=[[World Scientific]]
|pages=87–89
|year=2005
|isbn=978-981-238-244-3
}}</ref>


==Occurrence==
==Occurrence==

Revision as of 08:33, 28 November 2017

Chlorine-37, 37Cl
General
Symbol37Cl
Nameschlorine-37, 37Cl, Cl-37
Protons (Z)17
Neutrons (N)20
Nuclide data
Natural abundance24.23%
Half-life (t1/2)Stable
Isotopes of chlorine
Complete table of nuclides

Chlorine-37, or 37
Cl
, is one of the stable isotopes of chlorine, the other being chlorine-35 (35
Cl
). Its nucleus contains 17 protons and 20 neutrons for a total of 37 nucleons. Chlorine-37 accounts for 24.23% of natural chlorine, chlorine-35 accounting for 75.77%, giving chlorine atoms in bulk an apparent atomic weight of 35.453(2) g/mol.[1]

Remarkably, the Solar neutrinos were discovered by an experiment using a radiochemical method based on chlorine-37 transmutation.[2]

Neutrino detection

Main article: Homestake experiment

One of the historically important radiochemical methods of solar neutrino detection is based on inverse electron capture triggered by the absorption of an electron neutrino.[3] Chlorine-37 transmutes into Argon-37 via the reaction[4]

37
Cl
 +
ν
e → 37
Ar
 +
e−
.

Argon-37 then de-excites itself via electron capture (half-life = 35 d) into Chlorine-37 via the reaction

37
Ar
 +
e−
 → 37
Cl
 +
ν
e.

These last reactions involve Auger electrons of specific energies.[3][5] The detection of these electrons confirms that a neutrino event took place. Detection methods involve several hundred thousand liters of carbon tetrachloride (CCl4) or tetrachloroethylene (C2Cl4) stored in underground tanks.[2][3][6]

Occurrence

The representative terrestrial abundance of chlorine-37 is 24.22(4)% of chlorine atoms,[7] with a normal range of 24.14–24.36% of chlorine atoms. When measuring deviations in isotopic composition, the usual reference point is "Standard Mean Ocean Chloride" (SMOC), although a NIST Standard Reference Material (975a) also exists. SMOC is known to be around 24.219% chlorine-37 and to have an atomic weight of around 35.4525[8]

There is a known variation in the isotopic abundance of chlorine-37. This heavier isotope tends to be more prevalent in chloride minerals than in aqueous solutions such as sea water, although the isotopic composition of organochlorine compounds can vary in either direction from the SMOC standard in the range of several parts per thousand.[8]

See also

References

  1. ^ Wieser, M. E. (2006), "Atomic Weights of the Elements 2005" (PDF), Pure and Applied Chemistry, 78 (11): 2051–66, doi:10.1351/pac200678112051
  2. ^ a b J.N. Bahcall (1969). "Neutrinos from the Sun". Scientific American. 221 (1): 28–37. Bibcode:1969SciAm.221a..28B. doi:10.1038/scientificamerican0769-28.
  3. ^ a b c Sutton, Christine (1992). Spaceship Neutrino. Cambridge University Press. pp. 151–152. ISBN 978-0-521-36404-1. OCLC 25246163.
  4. ^ F.H. Shu (1982). The Physical Universe: An Introduction to Astronomy. University Science Books. p. 122. ISBN 978-0-935702-05-7.
  5. ^ A.H. Snell, F. Pleasonton (1955). "Spectrometry of the Neutrino Recoils of Argon-37". Physical Review. 100 (5): 1396–1403. Bibcode:1955PhRv..100.1396S. doi:10.1103/PhysRev.100.1396.
  6. ^ A. Bhatnagar, W. Livingston (2005). Fundamental of Solar Astronomy. World Scientific. pp. 87–89. ISBN 978-981-238-244-3.
  7. ^ Rosman, K. J. R.; Taylor, P. D. P. (1998), "Isotopic Compositions of the Elements 1997" (PDF), Pure and Applied Chemistry, 70 (1): 217–35, doi:10.1351/pac199870010217
  8. ^ a b de Laeter, J. R.; et al. (2003), "Atomic Weights of the Elements: Review 2000", Pure and Applied Chemistry, 75 (6): 683–800, doi:10.1351/pac200375060683
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