Isotopes of manganese

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Isotopes of manganese  (25Mn)
Main isotopes [1] Decay
abun­dance half-life (t1/2) mode pro­duct
52Mn synth 5.591 d β+ 52Cr
53Mn trace 3.7×106 y ε 53Cr
54Mnsynth312.081 dε 54Cr
β−54Fe
β+54Cr
55Mn100% stable
Standard atomic weight Ar°(Mn)
  • 54.938043±0.000002
  • 54.938±0.001 (abridged) [2] [3]

Naturally occurring manganese (25Mn) is composed of one stable isotope, 55Mn. 26 radioisotopes have been characterized, with the most stable being 53Mn with a half-life of 3.7 million years, 54Mn with a half-life of 312.3 days, and 52Mn with a half-life of 5.591 days. All of the remaining radioactive isotopes have half-lives that are less than 3 hours and the majority of these have half-lives that are less than a minute. This element also has 3 meta states.

Manganese is part of the iron group of elements, which are thought to be synthesized in large stars shortly before supernova explosions. 53Mn decays to 53 Cr with a half-life of 3.7 million years. Because of its relatively short half-life, 53Mn occurs only in tiny amounts due to the action of cosmic rays on iron in rocks. [4] Manganese isotopic contents are typically combined with chromium isotopic contents and have found application in isotope geology and radiometric dating. Mn−Cr isotopic ratios reinforce the evidence from 26Al and 107 Pd for the early history of the Solar System. Variations in 53Cr/52Cr and Mn/Cr ratios from several meteorites indicate an initial 53Mn/55Mn ratio that suggests Mn−Cr isotopic systematics must result from in-situ decay of 53Mn in differentiated planetary bodies. Hence 53Mn provides additional evidence for nucleosynthetic processes immediately before coalescence of the Solar System.

The isotopes of manganese range in atomic weight from 46  u (46Mn) to 72 u (72Mn). The primary decay mode before the most abundant stable isotope, 55Mn, is electron capture and the primary mode after is beta decay.

List of isotopes

Nuclide
[n 1] 		Z N Isotopic mass (Da)
[n 2] [n 3] 		Half-life
Decay
mode
[n 4] 		Daughter
isotope
[n 5] 		Spin and
parity
[n 6] [n 7] 		Natural abundance (mole fraction)
Excitation energy [n 7] Normal proportionRange of variation
46Mn252145.98672(12)#37(3) ms β+ (78%)46Cr(4+)
β+, p (22%)45V
β+, α (<1%)42Ti
β+, 2p (<1%)44Ti
46mMn150(100)# keV1# msβ+46Cr1-#
47Mn252246.97610(17)#100(50) msβ+ (96.6%)47Cr5/2−#
β+, p (3.4%)46V
48Mn252347.96852(12)158.1(22) msβ+ (99.71%)48Cr4+
β+, p (.027%)47V
β+, α (6×10−4%)44Ti
49Mn252448.959618(26)382(7) msβ+49Cr5/2−
50Mn252549.9542382(11)283.29(8) msβ+50Cr0+
50mMn229(7) keV1.75(3) minβ+50Cr5+
51Mn252650.9482108(11)46.2(1) minβ+51Cr5/2−
52Mn252751.9455655(21)5.591(3) dβ+52Cr6+
52mMn377.749(5) keV21.1(2) minβ+ (98.25%)52Cr2+
IT (1.75%)52Mn
53Mn252852.9412901(9)3.7(4)×106 y EC 53Cr7/2− trace
54Mn252953.9403589(14)312.03(3) dEC 99.99%54Cr3+
β− (2.9×10−4%)54Fe
β+ (5.76×10−7%)54Cr
55Mn253054.9380451(7)Stable5/2−1.0000
56Mn253155.9389049(7)2.5789(1) hβ−56Fe3+
57Mn253256.9382854(20)85.4(18) sβ−57Fe5/2−
58Mn253357.93998(3)3.0(1) sβ−58Fe1+
58mMn71.78(5) keV65.2(5) sβ− (>99.9%)58Fe(4)+
IT (<.1%)58Mn
59Mn253458.94044(3)4.59(5) sβ−59Fe(5/2)−
60Mn253559.94291(9)51(6) sβ−60Fe0+
60mMn271.90(10) keV1.77(2) sβ− (88.5%)60Fe3+
IT (11.5%)60Mn
61Mn253660.94465(24)0.67(4) sβ−61Fe(5/2)−
62Mn253761.94843(24)671(5) msβ− (>99.9%)62Fe(3+)
β−, n (<.1%)61Fe
62mMn0(150)# keV92(13) ms(1+)
63Mn253862.95024(28)275(4) msβ−63Fe5/2−#
64Mn253963.95425(29)88.8(25) msβ− (>99.9%)64Fe(1+)
β−, n (<.1%)63Fe
64mMn135(3) keV>100 µs
65Mn254064.95634(58)92(1) msβ− (>99.9%)65Fe5/2−#
β−, n (<.1%)64Fe
66Mn254165.96108(43)#64.4(18) msβ− (>99.9%)66Fe
β−, n (<.1%)65Fe
67Mn254266.96414(54)#45(3) msβ−67Fe5/2−#
68Mn254367.96930(64)#28(4) ms
69Mn254468.97284(86)#14(4) ms5/2−#
70Mn [5] 254569.978050(540)#19.9(17) msβ−=?70Fe(4,5)
β−, n? [n 8] 69Fe
β−, 2n? [n 8] 68Fe
71Mn [6] 254670.982160(540)#16# ms
(>400 ns)		β−? [n 8] 71Fe5/2-#
β−, n? [n 8] 70Fe
β−, 2n? [n 8] 69Fe
72Mn [7] 254771.988010(640)#12# ms
(>620 ns)		β−? [n 8] 72Fe
β−, n? [n 8] 71Fe
β−, 2n? [n 8] 70Fe
73Mn [8] 254872.992810(640)#12# ms
(>410 ns)		β−? [n 8] 73Fe5/2−#
This table header & footer:
  1. ↑ mMn – 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. ↑ Modes of decay:
    EC: Electron capture
    IT: Isomeric transition
    n: Neutron emission
    p: Proton emission
  5. ↑ Bold symbol as daughter – Daughter product is stable.
  6. ↑ ( ) spin value – Indicates spin with weak assignment arguments.
  7. 1 2 # – Values marked # are not purely derived from experimental data, but at least partly from trends of neighboring nuclides (TNN).
  8. 1 2 3 4 5 6 7 8 9 Decay mode shown is energetically allowed, but has not been experimentally observed to occur in this nuclide.

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References

  1. ↑ Kondev, 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.
  2. ↑ "Standard Atomic Weights: Manganese". CIAAW. 2017.
  3. ↑ Prohaska, Thomas; Irrgeher, Johanna; Benefield, Jacqueline; et al. (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.
  4. ↑ J. Schaefer; et al. (2006). "Terrestrial manganese-53 — A new monitor of Earth surface processes". Earth and Planetary Science Letters . 251 (3–4): 334–345. Bibcode:2006E&PSL.251..334S. doi:10.1016/j.epsl.2006.09.016.
  5. ↑ Tarasov, O. B.; et al. (April 2009). "Evidence for a Change in the Nuclear Mass Surface with the Discovery of the Most Neutron-Rich Nuclei with 17 ≤ Z ≤ 25". Physical Review Letters. 102 (14): 142501. arXiv: 0903.1975 . Bibcode:2009PhRvL.102n2501T. doi:10.1103/PhysRevLett.102.142501. PMID   19392430. S2CID   42329617 . Retrieved 29 January 2023.
  6. ↑ Ohnishi, Tetsuya; et al. (July 2010). "Identification of 45 New Neutron-Rich Isotopes Produced by In-Flight Fission of a 238U Beam at 345 MeV/nucleon". Journal of the Physical Society of Japan. 79 (7): 073201. arXiv: 1006.0305 . Bibcode:2010JPSJ...79g3201T. doi:10.1143/JPSJ.79.073201. S2CID   117037614 . Retrieved 29 January 2023.
  7. ↑ Tarasov, O. B.; et al. (May 2013). "Production cross sections from 82 Se fragmentation as indications of shell effects in neutron-rich isotopes close to the drip-line". Physical Review C. 87 (5): 054612. arXiv: 1303.7164 . Bibcode:2013PhRvC..87e4612T. doi:10.1103/PhysRevC.87.054612. S2CID   41501572 . Retrieved 29 January 2023.
  8. ↑ T. Sumikama; et al. (May 2017). "Observation of new neutron-rich Mn, Fe, Co, Ni, and Cu isotopes in the vicinity of 78 Ni". Physical Review C. 95 (5): 051601. Bibcode:2017PhRvC..95e1601S. doi:10.1103/PhysRevC.95.051601. hdl: 10261/161832 . Retrieved 29 January 2023.
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