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Isotopes of iron

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Isotopes ofiron (₂₆Fe)

Main isotopes^[1]			Decay
Isotope	abundance	half-life(t_1/2)	mode	product
⁵⁴Fe	5.85%	stable
⁵⁵Fe	synth	2.7562 y	ε	⁵⁵Mn
⁵⁶Fe	91.8%	stable
⁵⁷Fe	2.12%	stable
⁵⁸Fe	0.28%	stable
⁵⁹Fe	synth	44.50 d	β⁻	⁵⁹Co
⁶⁰Fe	trace	2.62×10⁶ y	β⁻	⁶⁰Co

Standard atomic weightA_r°(Fe)

55.845±0.002^[2]
55.845±0.002 (abridged)^[3]

Naturaliron (₂₆Fe) consists of four stableisotopes: 5.85%⁵⁴Fe, 91.75%⁵⁶Fe, 2.12%⁵⁷Fe and 0.28%⁵⁸Fe. There are 28 known radioisotopes and 8nuclear isomers, the most stable of which are⁶⁰Fe (half-life 2.62 million years) and⁵⁵Fe (half-life 2.7562 years).

Much of the past work on measuring the isotopic composition of iron has centered on determining⁶⁰Fe variations due to processes accompanyingnucleosynthesis (e.g.,meteorite studies) and ore formation. In the last decade however, advances inmass spectrometry technology have allowed the detection and quantification of minute, naturally occurring variations in the ratios of thestable isotopes of iron. Much of this work has been driven by theEarth andplanetary science communities, though applications to biological and industrial systems are beginning to emerge.^[4]

List of isotopes

[edit]

Nuclide ^{[n 1]}	Z	N	Isotopic mass(Da)^[5] ^{[n 2]}^{[n 3]}	Half-life^[1] ^{[n 4]}	Decay mode^[1] ^{[n 5]}	Daughter isotope ^{[n 6]}	Spin and parity^[1] ^{[n 7]}^{[n 4]}	Natural abundance(mole fraction)
Nuclide ^{[n 1]}	Excitation energy			Half-life^[1] ^{[n 4]}	Decay mode^[1] ^{[n 5]}	Daughter isotope ^{[n 6]}	Spin and parity^[1] ^{[n 7]}^{[n 4]}	Normal proportion^[1]	Range of variation
⁴⁵Fe	26	19	45.01547(30)#	2.5(2) ms	2p (70%)	⁴³Cr	3/2+#
					β⁺, p (18.9%)	⁴⁴Cr
					β⁺, 2p (7.8%)	⁴³V
					β⁺ (3.3%)	⁴⁵Mn
⁴⁶Fe	26	20	46.00130(32)#	13.0(20) ms	β⁺, p (78.7%)	⁴⁵Cr	0+
					β⁺ (21.3%)	⁴⁶Mn
					β⁺, 2p?	⁴⁴V
⁴⁷Fe	26	21	46.99235(54)#	21.9(2) ms	β⁺, p (88.4%)	⁴⁶Cr	7/2−#
⁴⁷Fe	26	21	46.99235(54)#	21.9(2) ms	β⁺ (11.6%)	⁴⁷Mn	7/2−#
⁴⁸Fe	26	22	47.980667(99)	45.3(6) ms	β⁺ (84.7%)	⁴⁸Mn	0+
⁴⁸Fe	26	22	47.980667(99)	45.3(6) ms	β⁺, p (15.3%)	⁴⁷Cr	0+
⁴⁹Fe	26	23	48.973429(26)	64.7(3) ms	β⁺, p (56.7%)	⁴⁸Cr	(7/2−)
⁴⁹Fe	26	23	48.973429(26)	64.7(3) ms	β⁺ (43.3%)	⁴⁹Mn	(7/2−)
⁵⁰Fe	26	24	49.9629880(90)	152.0(6) ms	β⁺	⁵⁰Mn	0+
⁵⁰Fe	26	24	49.9629880(90)	152.0(6) ms	β⁺, p?	⁴⁹Cr	0+
⁵¹Fe	26	25	50.9568551(15)	305.4(23) ms	β⁺	⁵¹Mn	5/2−
⁵²Fe	26	26	51.94811336(19)	8.275(8) h	β⁺	⁵²Mn	0+
^52mFe	6960.7(3) keV			45.9(6) s	β⁺ (99.98%)	⁵²Mn	12+
^52mFe	6960.7(3) keV			45.9(6) s	IT (0.021%)	⁵²Fe	12+
⁵³Fe	26	27	52.9453056(18)	8.51(2) min	β⁺	⁵³Mn	7/2−
^53mFe	3040.4(3) keV			2.54(2) min	IT	⁵³Fe	19/2−
⁵⁴Fe	26	28	53.93960819(37)	Observationally Stable^{[n 8]}			0+	0.05845(105)
^54mFe	6527.1(11) keV			364(7) ns	IT	⁵⁴Fe	10+
⁵⁵Fe	26	29	54.93829116(33)	2.7562(4) y	EC	⁵⁵Mn	3/2−
⁵⁶Fe^{[n 9]}	26	30	55.93493554(29)	Stable			0+	0.91754(106)
⁵⁷Fe	26	31	56.93539195(29)	Stable			1/2−	0.02119(29)
⁵⁸Fe	26	32	57.93327358(34)	Stable			0+	0.00282(12)
⁵⁹Fe	26	33	58.93487349(35)	44.500(12) d	β⁻	⁵⁹Co	3/2−
⁶⁰Fe	26	34	59.9340702(37)	2.62(4)×10⁶ y	β⁻	⁶⁰Co	0+	trace
⁶¹Fe	26	35	60.9367462(28)	5.98(6) min	β⁻	⁶¹Co	(3/2−)
^61mFe	861.67(11) keV			238(5) ns	IT	⁶¹Fe	9/2+
⁶²Fe	26	36	61.9367918(30)	68(2) s	β⁻	⁶²Co	0+
⁶³Fe	26	37	62.9402727(46)	6.1(6) s	β⁻	⁶³Co	(5/2−)
⁶⁴Fe	26	38	63.9409878(54)	2.0(2) s	β⁻	⁶⁴Co	0+
⁶⁵Fe	26	39	64.9450153(55)	805(10) ms	β⁻	⁶⁵Co	(1/2−)
⁶⁵Fe	26	39	64.9450153(55)	805(10) ms	β⁻,n?	⁶⁴Co	(1/2−)
^65m1Fe	393.7(2) keV			1.12(15) s	β⁻?	⁶⁵Co	(9/2+)
^65m2Fe	397.6(2) keV			418(12) ns	IT	⁶⁵Fe	(5/2+)
⁶⁶Fe	26	40	65.9462500(44)	467(29) ms	β⁻	⁶⁶Co	0+
⁶⁶Fe	26	40	65.9462500(44)	467(29) ms	β⁻, n?	⁶⁵Co	0+
⁶⁷Fe	26	41	66.9509300(41)	394(9) ms	β⁻	⁶⁷Co	(1/2-)
⁶⁷Fe	26	41	66.9509300(41)	394(9) ms	β⁻, n?	⁶⁶Co	(1/2-)
^67m1Fe	403(9) keV			64(17) μs	IT	⁶⁷Fe	(5/2+,7/2+)
^67m2Fe	450(100)# keV			75(21) μs	IT	⁶⁷Fe	(9/2+)
⁶⁸Fe	26	42	67.95288(21)#	188(4) ms	β⁻	⁶⁸Co	0+
⁶⁸Fe	26	42	67.95288(21)#	188(4) ms	β⁻, n?	⁶⁷Co	0+
⁶⁹Fe	26	43	68.95792(22)#	162(7) ms	β⁻	⁶⁹Co	1/2−#
					β⁻, n?	⁶⁸Co
					β⁻, 2n?	⁶⁷Co
⁷⁰Fe	26	44	69.96040(32)#	61.4(7) ms	β⁻	⁷⁰Co	0+
⁷⁰Fe	26	44	69.96040(32)#	61.4(7) ms	β⁻, n?	⁶⁹Co	0+
⁷¹Fe	26	45	70.96572(43)#	34.3(26) ms	β⁻	⁷¹Co	7/2+#
					β⁻, n?	⁷⁰Co
					β⁻, 2n?	⁶⁹Co
⁷²Fe	26	46	71.96860(54)#	17.0(10) ms	β⁻	⁷²Co	0+
					β⁻, n?	⁷¹Co
					β⁻, 2n?	⁷⁰Co
⁷³Fe	26	47	72.97425(54)#	12.9(16) ms	β⁻	⁷³Co	7/2+#
					β⁻, n?	⁷²Co
					β⁻, 2n?	⁷¹Co
⁷⁴Fe	26	48	73.97782(54)#	5(5) ms	β⁻	⁷⁴Co	0+
					β⁻, n?	⁷³Co
					β⁻, 2n?	⁷²Co
⁷⁵Fe	26	49	74.98422(64)#	9# ms [>620 ns]	β⁻?	⁷⁵Co	9/2+#
					β⁻, n?	⁷⁴Co
					β⁻, 2n?	⁷³Co
⁷⁶Fe	26	50	75.98863(64)#	3# ms [>410 ns]	β⁻?	⁷⁶Co	0+
This table header & footer: view

^^mFe – Excitednuclear 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).
^^a ^b# – 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⁺ to⁵⁴Cr with a half-life of over 4.4×10²⁰a^[6]
^Lowest mass per nucleon of all nuclides; End product of stellarnucleosynthesis

Iron-56

[edit]

Main article:Iron-56

⁵⁶Fe is the most abundant isotope of iron. It is also the isotope with the lowest mass per nucleon, 930.412 MeV/c², though not the isotope with the highestnuclear binding energy per nucleon, which isnickel-62.^[7] However, because of the details of how nucleosynthesis works,⁵⁶Fe is a more common endpoint of fusion insidesupernovae, where it is mostly produced as⁵⁶Ni, which subsequently decays to⁵⁶Co and then iron. Thus,⁵⁶Fe is more common in the universe, relative to otherheavy elements, including⁶²Ni,⁵⁸Fe, and⁶⁰Ni, all of which have a comparably high binding energy.

Iron-57

[edit]

⁵⁷Fe is widely used inMössbauer spectroscopy and the relatednuclear resonance vibrational spectroscopy due to the low natural variation in energy of the 14.4 keV nuclear transition.^[8] The transition was famously used to make the first definitive measurement ofgravitational redshift, in the 1960Pound–Rebka experiment.^[9]

Iron-60

[edit]

Iron-60 has a half-life of 2.62 million years,^[10] but was thought until 2009 to have a half-life of 1.5 million years. It undergoesbeta decay to⁶⁰Co, which then decays with the much shorter half-life of about 5 years to stable⁶⁰Ni.

In phases of the meteoritesSemarkona andChervony Kut, a correlation between the excess concentration of⁶⁰Ni, thegranddaughter isotope of⁶⁰Fe, and the abundance of the stable iron isotopes could be found, which is evidence for the existence of⁶⁰Fe at the time of formation of the Solar System.^[11] Depending on its original abundance, theenergy from the decay of⁶⁰Fe may have been significant, along with that of²⁶Al, to the remelting anddifferentiation ofasteroids andplanetesimals after their formation. These nickel abundances in extraterrestrial materials may also provide further insight into the origin of theSolar System and its early history.

Live (interstellar) iron-60 was first identified in deep sea sediments in 1999.^[12] These are deep seaferromanganese crusts, which are constantly growing, aggregating iron,manganese, and other elements.^[13] Iron-60 has been found in fossilized bacteria in sea floor sediments.^[14]^[15] In 2019, researchers found⁶⁰Fe inAntarctica.^[16] Iron-60 shows two peaks in deep sea sediments, the first 1.7–3.2 million years ago and the second 6.5–8.7 million years ago. The peaks are relate to the passage of the Solar System through theLocal Bubble and likely theOrion–Eridanus Superbubble. Thesesuperbubbles were created by multiplesupernovae.^[17] Traces of iron-60 have also been found in lunar samples.

The distance to the supernova of origin can be estimated by relating the amount of iron-60 intercepted as Earth passes through the expanding supernova ejecta. Assuming that the material ejected in a supernova expands uniformly out from its origin as a sphere with surface area 4πr². The fraction of the material intercepted by the Earth is dependent on its cross-sectional area (πR 2
Earth ) as it passes through the expanding debris:

$M_{\text{Fraction intercepted }}={\frac {\pi R_{\text{Earth }}^{2}}{4\pi r^{2}}}M_{ej}$

whereM_ej is the mass of ejected material. Assuming the intercepted material is distributed uniformly across the surface of the Earth (4πR 2
Earth ), the mass surface density (Σ_ej) of the supernova ejecta on Earth is:

$\Sigma _{ej}={\frac {M_{\text{Fraction intercepted }}}{A_{\text{surface,Earth }}}}={\frac {M_{ej}}{16\pi r^{2}}}$

The number of⁶⁰Fe atoms per unit area found on Earth can be estimated if the typical amount of⁶⁰Fe ejected from a supernova is known. This can be done by dividing the surface mass density (Σ_ej) by the atomic mass of⁶⁰Fe.

$N_{60}=\left({\frac {M_{ej,60}/m_{60}}{16\pi r^{2}}}\right)$

The equation forN⁶⁰ can be rearranged to find the distance to the supernova.

$r={\sqrt {\frac {M_{ej,60}}{16\pi m_{60}N_{60}}}}$

An example calculation for the distance to the supernova point of origin is given below. This calculation uses speculative values for terrestrial⁶⁰Fe atom surface density (N₆₀ ≈ 4 × 10¹¹ atoms/m²) and a rough estimate of the mass of⁶⁰Fe ejected by a supernova (10×10⁻⁵ M_☉).

${\begin{aligned}r&={\sqrt {\frac {10^{-5}M_{\odot }}{16\pi \left(60m_{p}\right)N_{60}}}}\\r&=3\times 10^{18}m=100pc\end{aligned}}$

More sophisticated analyses have been reported that take into consideration theflux and deposition of⁶⁰Fe as well as possible interfering background sources.^[18]

Cobalt-60, the decay product of iron-60, emits 1.173 MeV and 1.332 MeV gamma rays as it decays. These lines have long been important targets forgamma-ray astronomy, and have been detected by the gamma-ray observatoryINTEGRAL. The signal traces theGalactic plane, showing that⁶⁰Fe synthesis is ongoing in our galaxy, and probingelement production in massive stars.^[19]^[20]

References

[edit]

^^a ^b ^c ^d ^eKondev, F. G.; Wang, M.; Huang, W. J.; Naimi, S.; Audi, G. (2021)."The NUBASE2020 evaluation of nuclear properties"(PDF).Chinese Physics C.45 (3) 030001.doi:10.1088/1674-1137/abddae.
^"Standard Atomic Weights: Iron".CIAAW. 1993.
^Prohaska, Thomas; Irrgeher, Johanna; Benefield, Jacqueline; Böhlke, John K.; Chesson, Lesley A.; Coplen, Tyler B.; Ding, Tiping; Dunn, Philip J. H.; Gröning, Manfred; Holden, Norman E.; Meijer, Harro A. J. (2022-05-04)."Standard atomic weights of the elements 2021 (IUPAC Technical Report)".Pure and Applied Chemistry.doi:10.1515/pac-2019-0603.ISSN 1365-3075.
^N. Dauphas; O. Rouxel (2006). "Mass spectrometry and natural variations of iron isotopes".Mass Spectrometry Reviews.25 (4):515–550.Bibcode:2006MSRv...25..515D.doi:10.1002/mas.20078.PMID 16463281.
^Wang, Meng; Huang, W.J.; Kondev, F.G.; Audi, G.; Naimi, S. (2021). "The AME 2020 atomic mass evaluation (II). Tables, graphs and references*".Chinese Physics C.45 (3) 030003.doi:10.1088/1674-1137/abddaf.
^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.Bibcode:1998PhRvC..58.2566B.doi:10.1103/PhysRevC.58.2566.
^Fewell, M. P. (1995)."The atomic nuclide with the highest mean binding energy".American Journal of Physics.63 (7): 653.Bibcode:1995AmJPh..63..653F.doi:10.1119/1.17828.
^R. Nave."Mossbauer Effect in Iron-57".HyperPhysics. Georgia State University. Retrieved2009-10-13.
^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.
^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 the⁶⁰Fe Half-Life".Physical Review Letters.103 (7) 72502.Bibcode:2009PhRvL.103g2502R.doi:10.1103/PhysRevLett.103.072502.PMID 19792637.
^Mostefaoui, S.; Lugmair, G.W.; Hoppe, P.; El Goresy, A. (2004). "Evidence for live 60Fe in meteorites".New Astronomy Reviews.48 (1–4):155–59.Bibcode:2004NewAR..48..155M.doi:10.1016/j.newar.2003.11.022.
^Knie, K.; Korschinek, G.; Faestermann, T.; Wallner, C.; Scholten, J.; Hillebrandt, W. (1999-07-01)."Indication for Supernova Produced 60Fe Activity on Earth".Physical Review Letters.83 (1):18–21.Bibcode:1999PhRvL..83...18K.doi:10.1103/PhysRevLett.83.18.ISSN 0031-9007.
^Wallner, A.; Froehlich, M. B.; Hotchkis, M. A. C.; Kinoshita, N.; Paul, M.; Martschini, M.; Pavetich, S.; Tims, S. G.; Kivel, N.; Schumann, D.; Honda, M.; Matsuzaki, H.; Yamagata, T. (2021-05-01)."60Fe and 244Pu deposited on Earth constrain the r-process yields of recent nearby supernovae".Science.372 (6543):742–745.Bibcode:2021Sci...372..742W.doi:10.1126/science.aax3972.ISSN 0036-8075.PMID 33986180.
^Smith, Belinda (August 9, 2016)."Ancient bacteria store signs of supernova smattering".Cosmos.
^Ludwig, Peter; et al. (August 16, 2016)."Time-resolved 2-million-year-old supernova activity discovered in Earth's microfossil record".PNAS.113 (33):9232–9237.arXiv:1710.09573.Bibcode:2016PNAS..113.9232L.doi:10.1073/pnas.1601040113.PMC 4995991.PMID 27503888.
^Koll, Dominik; et al. (2019). "Interstellar⁶⁰Fe in Antarctica".Physical Review Letters.123 (7) 072701.Bibcode:2019PhRvL.123g2701K.doi:10.1103/PhysRevLett.123.072701.hdl:1885/298253.PMID 31491090.S2CID 201868513.
^Schulreich, M. M.; Feige, J.; Breitschwerdt, D. (2023-12-01)."Numerical studies on the link between radioisotopic signatures on Earth and the formation of the Local Bubble. II. Advanced modelling of interstellar 26Al, 53Mn, 60Fe, and 244Pu influxes as traces of past supernova activity in the solar neighbourhood".Astronomy and Astrophysics.680: A39.arXiv:2309.13983.Bibcode:2023A&A...680A..39S.doi:10.1051/0004-6361/202347532.ISSN 0004-6361.
^Ertel, Adrienne F.; Fry, Brian J.; Fields, Brian D.; Ellis, John (20 April 2023)."Supernova Dust Evolution Probed by Deep-sea 60Fe Time History".The Astrophysical Journal.947 (2):58–83.doi:10.3847/1538-4357/acb699.
^Harris, M. J.; Knödlseder, J.; Jean, P.; Cisana, E.; Diehl, R.; Lichti, G. G.; Roques, J.-P.; Schanne, S.; Weidenspointner, G. (2005-04-01)."Detection of γ-ray lines from interstellar 60Fe by the high resolution spectrometer SPI".Astronomy and Astrophysics.433 (3):L49–L52.arXiv:astro-ph/0502219.Bibcode:2005A&A...433L..49H.doi:10.1051/0004-6361:200500093.ISSN 0004-6361.
^Wang, W.; Siegert, T.; Dai, Z. G.; Diehl, R.; Greiner, J.; Heger, A.; Krause, M.; Lang, M.; Pleintinger, M. M. M.; Zhang, X. L. (2020-02-01)."Gamma-Ray Emission of 60Fe and 26Al Radioactivity in Our Galaxy".The Astrophysical Journal.889 (2): 169.arXiv:1912.07874.Bibcode:2020ApJ...889..169W.doi:10.3847/1538-4357/ab6336.ISSN 0004-637X.

Movatterモバイル変換

Isotopes of iron

List of isotopes

Iron-56

Iron-57

Iron-60

See also

References

Further reading

EC:	Electron capture
IT:	Isomeric transition
n:	Neutron emission
p:	Proton emission