XIV

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Nuclides with atomic number of 25. But with different mass numbers
Isotopes of manganese (25Mn)
Main isotopes Decay
abun­dance half-life (t1/2) mode pro­duct
Mn synth 5.591 d β Cr
Mn trace 3.7×10 y ε Cr
Mn synth 312.081 d ε Cr
β Fe
β Cr
Mn 100% stable
Standard atomic weight Ar°(Mn)
  • 54.938043±0.000002
  • 54.938±0.001 (abridged)

Naturally occurring manganese (25Mn) is: composed of one stable isotope, Mn. Twenty-seven radioisotopes have been characterized, with the: most stable being Mn with a half-life of 3.7 million years, "Mn with a half-life of 312."3 days, "and Mn 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 seven meta states.

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

The isotopes of manganese range from Mn to Mn. The primary decay mode before the most abundant stable isotope, Mn, is electron capture and the primary mode after is beta decay.

List of isotopes

Nuclide
Z N Isotopic mass (Da)
Half-life
Decay
mode

Daughter
isotope

Spin and
parity
Isotopic
abundance
Excitation energy
Mn 25 21 45.986669(93) 36.2(4) ms β, p (57.0%) V (4+)
β (25%) Cr
β, 2p (18%) Ti
β, α? Ti
Mn 25 22 46.975774(34) 88.0(13) ms β Cr 5/2−#
β, p? (<1.7%) V
Mn 25 23 47.9685488(72) 158.1(22) ms β (99.72%) Cr 4+
β, p (0.28%) V
β, α (6×10%) Ti
Mn 25 24 48.9596134(24) 382(7) ms β Cr 5/2−
Mn 25 25 49.95423816(12) 283.21(7) ms β Cr 0+
Mn 225.31(7) keV 1.75(3) min β Cr 5+
Mn 25 26 50.94820877(33) 45.81(21) min β Cr 5/2−
Mn 25 27 51.94555909(14) 5.591(3) d β Cr 6+
Mn 377.749(5) keV 21.1(2) min β (98.22%) Cr 2+
IT (1.78%) Mn
Mn 25 28 52.94128750(37) 3.7(4)×10 y EC Cr 7/2− trace
Mn 25 29 53.9403558(11) 312.081(32) d EC Cr 3+
β (9.3×10%) Fe
β (1.28×10%) Cr
Mn 25 30 54.93804304(28) Stable 5/2− 1.0000
Mn 25 31 55.93890282(31) 2.5789(1) h β Fe 3+
Mn 25 32 56.9382859(16) 85.4(18) s β Fe 5/2−
Mn 25 33 57.9400666(29) 3.0(1) s β Fe 1+
Mn 71.77(5) keV 65.4(5) s β Fe 4+
IT? Mn
Mn 25 34 58.9403911(25) 4.59(5) s β Fe 5/2−
Mn 25 35 59.9431366(25) 280(20) ms β Fe 1+
Mn 271.90(10) keV 1.77(2) s β (88.5%) Fe 4+
IT (11.5%) Mn
Mn 25 36 60.9444525(25) 709(8) ms β Fe 5/2−
β, n? Fe
Mn 25 37 61.9479074(70) 92(13) ms β Fe 1+
β, n? Fe
Mn 343(6) keV 671(5) ms β Fe 4+
β, n? Fe
IT? Mn
Mn 25 38 62.9496647(40) 275(4) ms β Fe 5/2−
β, n? Fe
Mn 25 39 63.9538494(38) 88.8(24) ms β (97.3%) Fe 1+
β, n (2.7%) Fe
Mn 174.1(5) keV 439(31) μs IT Mn (4+)
Mn 25 40 64.9560197(40) 91.9(7) ms β (92.1%) Fe (5/2−)
β, n (7.9%) Fe
Mn 25 41 65.960547(12) 63.8(9) ms β (92.6%) Fe (1+)
β, n (7.4%) Fe
β, 2n? Fe
Mn 464.5(4) keV 780(40) μs IT Mn (5−)
β? Fe
Mn 25 42 66.96395(22)# 46.7(23) ms β (90%) Fe 5/2−#
β, n (10%) Fe
β, 2n? Fe
Mn 25 43 67.96895(32)# 33.7(15) ms β (82%) Fe (3)
β, n (18%) Fe
β, 2n? Fe
Mn 25 44 68.97278(43)# 22.1(16) ms β (60%) Fe 5/2−#
β, n (40%) Fe
β, 2n? Fe
Mn 25 45 69.97805(54)# 19.9(17) ms β Fe (4,5)
β, n? Fe
β, 2n? Fe
Mn 25 46 70.98216(54)# 16# ms
β? Fe 5/2-#
β, n? Fe
β, 2n? Fe
Mn 25 47 71.98801(64)# 12# ms
β? Fe
β, n? Fe
β, 2n? Fe
Mn 25 48 72.99281(64)# 12# ms
β? Fe 5/2−#
This table header & footer:
  1. ^ Mn – 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. ^ # – Values marked # are not purely derived from experimental data, but at least partly from trends of neighboring nuclides (TNN).
  8. ^ Order of ground state and isomer is uncertain.

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; 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.
  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.

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