Isotopes of iron

Main isotopes of iron
Iso­tope Decay
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 syn 2.6×106 y β 60Co
Standard atomic weight (Ar)

Naturally occurring iron (26Fe) consists of four stable isotopes: 5.845% of 54Fe (possibly radioactive with a half-life over 3.1×1022 years), 91.754% of 56Fe, 2.119% of 57Fe and 0.282% of 58Fe. There are 24 known radioactive isotopes and their half-lives are shown below. See Brookhaven National Laboratory Interactive Table of Nuclides for a more accurate reading.

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.[2]

Iron-54

54Fe is observationally stable, but theoretically can decay to 54Cr, with a half-life of more than 3.1x1022 years via double electron capture (εε).

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.[3] 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.[4] The transition was famously used to make the first definitive measurement of gravitational redshift, in the 1960 Pound-Rebka experiment.[5]

Iron-60

Iron-60 is an iron isotope with a half-life of 2.6 million years,[6][7] but was thought until 2009 to have a half-life of 1.5 million years. It undergoes beta decay to cobalt-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.

Remnants of Iron-60 found in fossilised bacteria in sea floor sediments suggest there was a supernova in the vicinity of the solar system approx 2 million years ago.[8][9]

List of isotopes

nuclide
symbol
Z(p) N(n)  
Atomic mass (u)
 
half-life decay
mode(s)[10][n 1]
daughter
isotope(s)[n 2]
nuclear
spin
representative
isotopic
composition
(mole fraction)
range of natural
variation
(mole fraction)
excitation energy
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 3] 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 4] 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. Abbreviations:
    EC: Electron capture
    IT: Isomeric transition
  2. Bold for stable isotopes
  3. Believed to decay by β+β+ to 54Cr with a half-life of over 3.1×1022 a
  4. Lowest mass per nucleon of all nuclides; End product of stellar nucleosynthesis

Notes

See also

References

  1. Meija, J.; et al. (2016). "Atomic weights of the elements 2013 (IUPAC Technical Report)". Pure Appl. Chem. 88 (3): 265–91. doi:10.1515/pac-2015-0305.
  2. N. Dauphas; O. Rouxel (2006). "Mass spectrometry and natural variations of iron isotopes". Mass Spectrometry Reviews. 25 (4): 515–550. PMID 16463281. doi:10.1002/mas.20078.
  3. Fewell, M. P. "The atomic nuclide with the highest mean binding energy". American Journal of Physics 63 (7): 653-58. Accessed: 2011-03-22. (Archived by WebCite® at https://www.webcitation.org/5xNHry2gq)
  4. R. Nave. "Mossbauer Effect in Iron-57". HyperPhysics. Georgia State University. Retrieved 2009-10-13.
  5. Pound, R. V.; Rebka Jr. G. A. (April 1, 1960). "Apparent weight of photons". Physical Review Letters. 4 (7): 337–341. Bibcode:1960PhRvL...4..337P. doi:10.1103/PhysRevLett.4.337.
  6. Rugel, G.; Faestermann, T.; Knie, K.; Korschinek, G.; Poutivtsev, M.; Schumann, D.; Kivel, N.; Günther-Leopold, I.; Weinreich, R.; Wohlmuther, M. (2009). "New Measurement of the 60Fe Half-Life". Physical Review Letters. 103 (7): 72502. Bibcode:2009PhRvL.103g2502R. doi:10.1103/PhysRevLett.103.072502.
  7. "Eisen mit langem Atem".
  8. Ancient bacteria store signs of supernova smattering
  9. Ocean sediment sample holds iron believed to be from a supernova. Aug 2016
  10. "Universal Nuclide Chart". nucleonica. (Registration required (help)).
  11. M. Wang, G. Audi, A. H. Wapstra, F. G. Kondev, M. MacCormick, X. Xu, and B. Pfeiffer (2012), "The AME2012 atomic mass evaluation (II). Tables, graphs and references", Chinese Physics C, Vol. 36, 1603-2014.

Further reading

Isotopes of manganese Isotopes of iron Isotopes of cobalt
Table of nuclides
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