Isotopes of iron

Short description: Nuclides with atomic number of 26 but with different mass numbers

Main isotopes of Chemistry:iron (26Fe) | Iso­tope | Decay

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| abun­dance | half-life (t1/2) | mode | pro­duct
54Fe  | 5.85%  | stable
55Fe | syn | 2.73 y  | ε | 55Mn
56Fe | 91.75%  | stable
57Fe  | 2.12%  | stable
58Fe  | 0.28%  | stable
59Fe  | syn  | 44.6 d  | β− | 59Co
60Fe  | trace | 2.6×106 y  | β− | 60Co
Standard atomic weight Ar, standard(Fe)|

* 55.845(2)[1]

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Naturally occurring iron (26Fe) consists of four stable isotopes: 5.845% of 54Fe (possibly radioactive with a half-life over 4.4×1020 years),[2] 91.754% of 56Fe, 2.119% of 57Fe and 0.286% of 58Fe. There are 24 known radioactive isotopes, the most stable of which are 60Fe (half-life 2.6 million years) and 55Fe (half-life 2.7 years).

Much of the past work on measuring the isotopic composition of Fe has centered on determining 60Fe variations due to processes accompanying nucleosynthesis (i.e., meteorite studies) and ore formation. In the last decade however, advances in mass spectrometry technology have allowed the detection and quantification of minute, naturally occurring variations in the ratios of the stable isotopes of iron. Much of this work has been driven by the Earth and planetary science communities, although applications to biological and industrial systems are beginning to emerge.[3]

## Contents

* 1 List of isotopes
* 2 Iron-54
* 3 Iron-56
* 4 Iron-57
* 5 Iron-58
* 6 Iron-60
* 7 References
* 8 Further reading

## List of isotopes

Nuclide
[n 1] | Z | N | Isotopic mass (u)
[n 2][n 3] | Half-life
[n 4] | Decay
mode
[n 5] | Daughter
isotope
[n 6] | Spin and
parity
[n 7][n 4] | Physics:Natural abundance (mole fraction)

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Excitation energy  | Normal proportion  | Range of variation
45Fe  | 26  | 19  | 45.01458(24)#  | 1.89(49) ms  | β+ (30%)  | 45Mn  | 3/2+#  |  |
2p (70%)  | 43Cr
46Fe  | 26  | 20  | 46.00081(38)#  | 9(4) ms
[12(+4-3) ms]  | β+ (>99.9%)  | 46Mn  | 0+  |  |
β+, p (<.1%)  | 45Cr
47Fe  | 26  | 21  | 46.99289(28)#  | 21.8(7) ms  | β+ (>99.9%)  | 47Mn  | 7/2−#  |  |
β+, p (<.1%)  | 46Cr
48Fe  | 26  | 22  | 47.98050(8)#  | 44(7) ms  | β+ (96.41%)  | 48Mn  | 0+  |  |
β+, p (3.59%)  | 47Cr
49Fe  | 26  | 23  | 48.97361(16)#  | 70(3) ms  | β+, p (52%)  | 48Cr  | (7/2−)  |  |
β+ (48%)  | 49Mn
50Fe  | 26  | 24  | 49.96299(6)  | 155(11) ms  | β+ (>99.9%)  | 50Mn  | 0+  |  |
β+, p (<.1%)  | 49Cr
51Fe  | 26  | 25  | 50.956820(16)  | 305(5) ms  | β+ | 51Mn  | 5/2−  |  |
52Fe  | 26  | 26  | 51.948114(7)  | 8.275(8) h  | β+ | 52mMn  | 0+  |  |
52mFe  | 6.81(13) MeV  | 45.9(6) s  | β+ | 52Mn  | (12+)#  |  |
53Fe  | 26  | 27  | 52.9453079(19)  | 8.51(2) min  | β+ | 53Mn  | 7/2−  |  |
53mFe  | 3040.4(3) keV  | 2.526(24) min  | IT  | 53Fe  | 19/2−  |  |
54Fe  | 26  | 28  | 53.9396090(5)  | Observationally Stable[n 8] | 0+  | 0.05845(35)  | 0.05837–0.05861
54mFe  | 6526.9(6) keV  | 364(7) ns  |  |  | 10+  |  |
55Fe | 26  | 29  | 54.9382934(7)  | 2.737(11) y  | EC | 55Mn | 3/2−  |  |
56Fe[n 9] | 26  | 30  | 55.9349363(5)  | Stable | 0+  | 0.91754(36)  | 0.91742–0.91760
57Fe  | 26  | 31  | 56.9353928(5)  | Stable | 1/2−  | 0.02119(10)  | 0.02116–0.02121
58Fe  | 26  | 32  | 57.9332744(5)  | Stable | 0+  | 0.00282(4)  | 0.00281–0.00282
59Fe  | 26  | 33  | 58.9348755(8)  | 44.495(9) d  | β− | 59Co | 3/2−  |  |
60Fe  | 26  | 34  | 59.934072(4)  | 2.6×106 y  | β− | 60Co  | 0+  | trace |
61Fe  | 26  | 35  | 60.936745(21)  | 5.98(6) min  | β− | 61Co  | 3/2−,5/2−  |  |
61mFe  | 861(3) keV  | 250(10) ns  |  |  | 9/2+#  |  |
62Fe  | 26  | 36  | 61.936767(16)  | 68(2) s  | β− | 62Co  | 0+  |  |
63Fe  | 26  | 37  | 62.94037(18)  | 6.1(6) s  | β− | 63Co  | (5/2)−  |  |
64Fe  | 26  | 38  | 63.9412(3)  | 2.0(2) s  | β− | 64Co  | 0+  |  |
65Fe  | 26  | 39  | 64.94538(26)  | 1.3(3) s  | β− | 65Co  | 1/2−#  |  |
65mFe  | 364(3) keV  | 430(130) ns  |  |  | (5/2−)  |  |
66Fe  | 26  | 40  | 65.94678(32)  | 440(40) ms  | β− (>99.9%)  | 66Co  | 0+  |  |
β−, n (<.1%)  | 65Co
67Fe  | 26  | 41  | 66.95095(45)  | 394(9) ms  | β− (>99.9%)  | 67Co  | 1/2−#  |  |
β−, n (<.1%)  | 66Co
67mFe  | 367(3) keV  | 64(17) µs |  |  | (5/2−)  |  |
68Fe  | 26  | 42  | 67.95370(75)  | 187(6) ms  | β− (>99.9%)  | 68Co  | 0+  |  |
β−, n  | 67Co
69Fe  | 26  | 43  | 68.95878(54)#  | 109(9) ms  | β− (>99.9%)  | 69Co  | 1/2−#  |  |
β−, n (<.1%)  | 68Co
70Fe  | 26  | 44  | 69.96146(64)#  | 94(17) ms  |  |  | 0+  |  |
71Fe  | 26  | 45  | 70.96672(86)#  | 30# ms
[>300 ns]  |  |  | 7/2+#  |  |
72Fe  | 26  | 46  | 71.96962(86)#  | 10# ms
[>300 ns]  |  |  | 0+  |  |

1. ↑ mFe - Excited nuclear isomer.
2. ↑ ( ) - Uncertainty (1σ) is given in concise form in parentheses after the corresponding last digits.
3. ↑ # - Atomic mass marked #: value and uncertainty derived not from purely experimental data, but at least partly from trends from the Mass Surface (TMS).
4. ↑ 4.0 4.1 # - Values marked # are not purely derived from experimental data, but at least partly from trends of neighboring nuclides (TNN).
5. ↑ Modes of decay:  EC: | Electron capture

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IT: | Isomeric transition
n: | Neutron emission
p: | Proton emission
6. ↑ Bold symbol as daughter - Daughter product is stable.
7. ↑ ( ) spin value - Indicates spin with weak assignment arguments.
8. ↑ Believed to decay by β+β+ to 54Cr with a half-life of over 4.4×1020 a[2]
9. ↑ Lowest mass per nucleon of all nuclides; End product of stellar nucleosynthesis

* Atomic masses of the stable nuclides (54Fe, 56Fe, 57Fe, and 58Fe) are given by the AME2012 atomic mass evaluation. The one standard deviation errors are given in parentheses after the corresponding last digits.[4]

## Iron-54

54Fe is observationally stable, but theoretically can decay to 54Cr, with a half-life of more than 4.4×1020 years via double electron capture (εε).[2]

## Iron-56

Main page: Physics:Iron-56

The isotope 56Fe is the isotope with the lowest mass per nucleon, 930.412 MeV/c2, though not the isotope with the highest nuclear binding energy per nucleon, which is nickel-62.[5] However, because of the details of how nucleosynthesis works, 56Fe is a more common endpoint of fusion chains inside extremely massive stars and is therefore more common in the universe, relative to other metals, including 62Ni, 58Fe and 60Ni, all of which have a very high binding energy.

## Iron-57

The isotope 57Fe is widely used in Mössbauer spectroscopy and the related nuclear resonance vibrational spectroscopy due to the low natural variation in energy of the 14.4 keV nuclear transition.[6] The transition was famously used to make the first definitive measurement of gravitational redshift, in the 1960 Pound-Rebka experiment.[7]

## Iron-58

## Iron-60

Iron-60 is an iron isotope with a half-life of 2.6 million years,[8][9] but was thought until 2009 to have a half-life of 1.5 million years. It undergoes beta decay to cobalt-60, which then decays with a half-life of about 5 years to stable nickel-60. Traces of iron-60 have been found in lunar samples.

In phases of the meteorites Semarkona and Chervony Kut, a correlation between the concentration of 60Ni, the granddaughter isotope of 60Fe, and the abundance of the stable iron isotopes could be found, which is evidence for the existence of 60Fe at the time of formation of the Solar System. Possibly the energy released by the decay of 60Fe contributed, together with the energy released by decay of the radionuclide 26Al, to the remelting and differentiation of asteroids after their formation 4.6 billion years ago. The abundance of 60Ni present in extraterrestrial material may also provide further insight into the origin of the Solar System and its early history.

Iron-60 found in fossilised bacteria in sea floor sediments suggest there was a supernova in the vicinity of the Solar System approximately 2 million years ago.[10][11] Iron-60 is also found in sediments from 8 million years ago.[12]

In 2019, researchers found interstellar 60Fe in Antarctica, which they relate to the Local Interstellar Cloud.[13]

## References

1. ↑ Meija, Juris; Coplen, Tyler B.; Berglund, Michael; Brand, Willi A.; De Bièvre, Paul; Gröning, Manfred; Holden, Norman E.; Irrgeher, Johanna et al. (2016). "Atomic weights of the elements 2013 (IUPAC Technical Report)". Pure and Applied Chemistry 88 (3): 265–91. doi:10.1515/pac-2015-0305.
2. ↑ 2.0 2.1 2.2 Bikit, I.; Krmar, M.; Slivka, J.; Vesković, M.; Čonkić, Lj.; Aničin, I. (1998). "New results on the double β decay of iron". Physical Review C 58 (4): 2566–2567. doi:10.1103/PhysRevC.58.2566. Bibcode: 1998PhRvC..58.2566B.
3. ↑ N. Dauphas; O. Rouxel (2006). "Mass spectrometry and natural variations of iron isotopes". Mass Spectrometry Reviews 25 (4): 515–550. doi:10.1002/mas.20078. PMID 16463281. Bibcode: 2006MSRv...25..515D.
4. ↑ Wang, M.; Audi, G.; Wapstra, A.H.; Kondev, F.G.; MacCormick, M.; Xu, X.; Pfeiffer, B. (2012). "The Ame2012 atomic mass evaluation". Chinese Physics C 36 (12): 1603–2014. doi:10.1088/1674-1137/36/12/003. Bibcode: 2012ChPhC..36....3M.
5. ↑ Fewell, M. P. (1995). "The atomic nuclide with the highest mean binding energy". American Journal of Physics 63 (7): 653. doi:10.1119/1.17828. Bibcode: 1995AmJPh..63..653F. https://ui.adsabs.harvard.edu/abs/1995AmJPh..63..653F/abstract.
6. ↑ R. Nave. "Mossbauer Effect in Iron-57". HyperPhysics. Georgia State University. http://hyperphysics.phy-astr.gsu.edu/Hbase/Nuclear/mossfe.html.
7. ↑ Pound, R. V.; Rebka Jr. G. A. (April 1, 1960). "Apparent weight of photons". Physical Review Letters 4 (7): 337–341. doi:10.1103/PhysRevLett.4.337. Bibcode: 1960PhRvL...4..337P.
8. ↑ Rugel, G.; Faestermann, T.; Knie, K.; Korschinek, G.; Poutivtsev, M.; Schumann, D.; Kivel, N.; Günther-Leopold, I. et al. (2009). "New Measurement of the 60Fe Half-Life". Physical Review Letters 103 (7): 72502. doi:10.1103/PhysRevLett.103.072502. PMID 19792637. Bibcode: 2009PhRvL.103g2502R. https://www.dora.lib4ri.ch/psi/islandora/object/psi:17743.
9. ↑ "Eisen mit langem Atem". scienceticker. 27 August 2009. http://www.scienceticker.info/2009/08/27/eisen-mit-langem-atem/#more-5677.
10. ↑ Belinda Smith (Aug 9, 2016). "Ancient bacteria store signs of supernova smattering". Cosmos. https://cosmosmagazine.com/space/ancient-bacteria-store-signs-of-supernova-smattering.
11. ↑ Peter Ludwig (Aug 16, 2016). "Time-resolved 2-million-year-old supernova activity discovered in Earth's microfossil record". PNAS 113 (33): 9232–9237. doi:10.1073/pnas.1601040113. PMID 27503888. Bibcode: 2016PNAS..113.9232L.
12. ↑ Colin Barras (Oct 14, 2017). "Fires may have given our evolution a kick-start". New Scientist 236 (3147): 7. doi:10.1016/S0262-4079(17)31997-8. Bibcode: 2017NewSc.236....7B. https://www.newscientist.com/article/mg23631474-400-exploding-stars-could-have-kickstarted-our-ancestors-evolution/.
13. ↑ Koll, Dominik; et., al. (2019). "Interstellar 60Fe in Antarctica". Physical Review Letters 123 (7): 072701. doi:10.1103/PhysRevLett.123.072701. PMID 31491090. Bibcode: 2019PhRvL.123g2701K.

Isotope masses from:

* Audi, Georges; Bersillon, Olivier; Blachot, Jean; Wapstra, Aaldert Hendrik (2003), "The NUBASE evaluation of nuclear and decay properties", Nuclear Physics A 729: 3–128, doi:10.1016/j.nuclphysa.2003.11.001, Bibcode: 2003NuPhA.729....3A, https://hal.archives-ouvertes.fr/in2p3-00020241/document

Isotopic compositions and standard atomic masses from:

* Wieser, Michael E. (2006). "Atomic weights of the elements 2005 (IUPAC Technical Report)". Pure and Applied Chemistry 78 (11): 2051–2066. doi:10.1351/pac200678112051.

Half-life, spin, and isomer data selected from:

* Audi, Georges; Bersillon, Olivier; Blachot, Jean; Wapstra, Aaldert Hendrik (2003), "The NUBASE evaluation of nuclear and decay properties", Nuclear Physics A 729: 3–128, doi:10.1016/j.nuclphysa.2003.11.001, Bibcode: 2003NuPhA.729....3A, https://hal.archives-ouvertes.fr/in2p3-00020241/document
* National Nuclear Data Center. "NuDat 2.x database". Brookhaven National Laboratory. http://www.nndc.bnl.gov/nudat2/.
* Lide, David R., ed (2004). "11. Table of the Isotopes". CRC Handbook of Chemistry and Physics (85th ed.). Boca Raton, Florida: CRC Press. ISBN 978-0-8493-0485-9.

## Further reading

* J. M. Nielsen (1960). The Radiochemistry of Iron. National Academy of Sciences/National Research Council. http://library.lanl.gov/cgi-bin/getfile?rc000015.pdf.

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Isotopes of the chemical elements

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* Table of nuclides
* Categories: Isotopes
* Tables of nuclides
* Metastable isotopes
* Isotopes by element

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