Name, symbol Chlorine-37,37Cl
Neutrons 20
Protons 17
Nuclide data
Natural abundance 24.23%
Half-life Stable

Chlorine-37, or 37
, is one of the stable isotopes of chlorine, the other being chlorine-35 (35
). 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.[1]

Chlorine-37 is routinely used in neutrino detection experiments, such as those going on at the Sudbury Neutrino Observatory or at the Super-Kamiokande.[2]


Neutrino detection

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]

+ ν
+ e

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

+ e
+ ν

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 usually involve several thousand liters of carbon tetrachloride (CCl4) or tetrachloroethylene (C2Cl4) stored in underground tanks.[2][3][6]


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


  1. ^ International Union of Pure and Applied Chemistry (2006), "Atomic Weights of the Elements 2005", Pure Appl. Chem. 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. doi:10.1038/scientificamerican0769-28. 
  3. ^ a b c C. Sutton (1992). Spaceship Neutrino. Cambridge University Press. pp. 151–152. ISBN 0-531-36404-3. 
  4. ^ F.H. Shu (1982). The Physical Universe: An Introduction to Astronomy. University Science Books. p. 122. ISBN 0-935702-05-9. 
  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 981-238-244-5. 
  7. ^ International Union of Pure and Applied Chemistry (1998), "Isotopic Compositions of the Elements 1997", Pure Appl. Chem. 70 (1): 217–35, doi:10.1351/pac199870010217, 
  8. ^ a b International Union of Pure and Applied Chemistry (2003), "Atomic Weights of the Elements: Review 2000", Pure Appl. Chem. 75 (6): 683–800, doi:10.1351/pac200375060683 

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