Isotopes of iron

Main isotopes of Chemistry:iron (₂₆Fe)
Standard atomic weight Ar, standard(Fe)	55.845(2);
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Short description: Nuclides with atomic number of 26 but with different mass numbers

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]

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)
Nuclide ^{[n 1]}	Excitation energy			Half-life ^{[n 4]}	Decay mode ^{[n 5]}	Daughter isotope ^{[n 6]}	Spin and parity ^{[n 7]}^{[n 4]}	Normal proportion	Range of variation
⁴⁵Fe	26	19	45.01458(24)#	1.89(49) ms	β⁺ (30%)	⁴⁵Mn	3/2+#
⁴⁵Fe	26	19	45.01458(24)#	1.89(49) ms	2p (70%)	⁴³Cr	3/2+#
⁴⁶Fe	26	20	46.00081(38)#	9(4) ms [12(+4-3) ms]	β⁺ (>99.9%)	⁴⁶Mn	0+
⁴⁶Fe	26	20	46.00081(38)#	9(4) ms [12(+4-3) ms]	β⁺, p (<.1%)	⁴⁵Cr	0+
⁴⁷Fe	26	21	46.99289(28)#	21.8(7) ms	β⁺ (>99.9%)	⁴⁷Mn	7/2−#
⁴⁷Fe	26	21	46.99289(28)#	21.8(7) ms	β⁺, p (<.1%)	⁴⁶Cr	7/2−#
⁴⁸Fe	26	22	47.98050(8)#	44(7) ms	β⁺ (96.41%)	⁴⁸Mn	0+
⁴⁸Fe	26	22	47.98050(8)#	44(7) ms	β⁺, p (3.59%)	⁴⁷Cr	0+
⁴⁹Fe	26	23	48.97361(16)#	70(3) ms	β⁺, p (52%)	⁴⁸Cr	(7/2−)
⁴⁹Fe	26	23	48.97361(16)#	70(3) ms	β⁺ (48%)	⁴⁹Mn	(7/2−)
⁵⁰Fe	26	24	49.96299(6)	155(11) ms	β⁺ (>99.9%)	⁵⁰Mn	0+
⁵⁰Fe	26	24	49.96299(6)	155(11) ms	β⁺, p (<.1%)	⁴⁹Cr	0+
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+
⁶⁶Fe	26	40	65.94678(32)	440(40) ms	β⁻, n (<.1%)	⁶⁵Co	0+
⁶⁷Fe	26	41	66.95095(45)	394(9) ms	β⁻ (>99.9%)	⁶⁷Co	1/2−#
⁶⁷Fe	26	41	66.95095(45)	394(9) ms	β⁻, n (<.1%)	⁶⁶Co	1/2−#
^67mFe	367(3) keV			64(17) µs			(5/2−)
⁶⁸Fe	26	42	67.95370(75)	187(6) ms	β⁻ (>99.9%)	⁶⁸Co	0+
⁶⁸Fe	26	42	67.95370(75)	187(6) ms	β⁻, n	⁶⁷Co	0+
⁶⁹Fe	26	43	68.95878(54)#	109(9) ms	β⁻ (>99.9%)	⁶⁹Co	1/2−#
⁶⁹Fe	26	43	68.95878(54)#	109(9) ms	β⁻, n (<.1%)	⁶⁸Co	1/2−#
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+

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

EC: Electron capture

IT: Isomeric transition

n: Neutron emission

p: Proton emission
↑ Bold symbol as daughter – Daughter product is stable.
↑ ( ) spin value – Indicates spin with weak assignment arguments.
↑ Believed to decay by β⁺β⁺ to ⁵⁴Cr with a half-life of over 4.4×10²⁰ a^[2]
↑ 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-58 is a stable isotope of iron. It can be used to combat anemia and low iron absorption, to metabolically track iron-controlling human genes, and for tracing elements in nature.^[8]^[9] Iron-58 is also an assisting reagent in the synthesis of superheavy elements.^[9]

Iron-60

Iron-60 is an iron isotope with a half-life of 2.6 million years,^[10]^[11] 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.^[12]^[13] Iron-60 is also found in sediments from 8 million years ago.^[14]

In 2019, researchers found interstellar ⁶⁰Fe in Antarctica, which they relate to the Local Interstellar Cloud.^[15]

References

↑ 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.
↑ ^2.0 ^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.
↑ 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.
↑ 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.
↑ 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.
↑ R. Nave. "Mossbauer Effect in Iron-57". HyperPhysics. Georgia State University. http://hyperphysics.phy-astr.gsu.edu/Hbase/Nuclear/mossfe.html.
↑ 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.
↑ "Iron-58 Metal Isotope" (in en). https://www.americanelements.com/iron-58-metal-isotope-13968-47-3.
↑ ^9.0 ^9.1 Vasiliev, Petr. "Iron-58, Iron-58 Isotope, Enriched Iron-58, Iron-58 Metal" (in en). https://www.buyisotope.com/iron-58-isotope.php.
↑ 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%3A17743.
↑ "Eisen mit langem Atem". scienceticker. 27 August 2009. http://www.scienceticker.info/2009/08/27/eisen-mit-langem-atem/#more-5677.
↑ Belinda Smith (Aug 9, 2016). "Ancient bacteria store signs of supernova smattering". Cosmos. https://cosmosmagazine.com/space/ancient-bacteria-store-signs-of-supernova-smattering.
↑ 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.
↑ 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/.
↑ 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.