# Isotopes of nickel

Naturally occurring nickel ($_{28}$Ni) is composed of five stable isotopes; $^{58}$ Ni , $^{60}$ Ni , $^{61}$ Ni , $^{62}$ Ni and $^{64}$ Ni , with $^{58}$ Ni being the most abundant (68.077% natural abundance). 26 radioisotopes have been characterised with the most stable being $^{59}$ Ni with a half-life of 81,000 years, $^{63}$ Ni with a half-life of 100.1 years, and $^{56}$ Ni with a half-life of 6.077 days. All of the remaining radioactive isotopes have half-lives that are less than 60 hours and the majority of these have half-lives that are less than 30 seconds. This element also has 8 meta states.

## List of isotopes

| Nuclide | Z | N | Isotopic mass (Da) | Half-life | Decay mode | Daughter isotope | Spin and parity | Natural abundance (mole fraction) | Natural abundance (mole fraction) |
| Nuclide | Excitation energy | Excitation energy | Excitation energy | Half-life | Decay mode | Daughter isotope | Spin and parity | Normal proportion | Range of variation |
| $^{48}$ Ni | 28 | 20 | 48.01952(46)# | 2.8(8) ms | 2p (70%) | $^{46}$ Fe | 0+ | | |
| $^{48}$ Ni | 28 | 20 | 48.01952(46)# | 2.8(8) ms | β$^+$ (30%) | $^{48}$ Co | 0+ | | |
| $^{48}$ Ni | 28 | 20 | 48.01952(46)# | 2.8(8) ms | β$^+$, p? | $^{47}$ Fe | 0+ | | |
| $^{49}$ Ni | 28 | 21 | 49.00916(64)# | 7.5(10) ms | β$^+$, p (83%) | $^{48}$ Fe | 7/2−# | | |
| $^{49}$ Ni | 28 | 21 | 49.00916(64)# | 7.5(10) ms | β$^+$ (17%) | $^{49}$ Co | 7/2−# | | |
| $^{50}$ Ni | 28 | 22 | 49.99629(54)# | 18.5(12) ms | β$^+$, p (73%) | $^{49}$ Fe | 0+ | | |
| $^{50}$ Ni | 28 | 22 | 49.99629(54)# | 18.5(12) ms | β$^+$, 2p (14%) | $^{48}$ Mn | 0+ | | |
| $^{50}$ Ni | 28 | 22 | 49.99629(54)# | 18.5(12) ms | β$^+$ (13%) | $^{50}$ Co | 0+ | | |
| $^{51}$ Ni | 28 | 23 | 50.98749(54)# | 23.8(2) ms | β$^+$, p (87.2%) | $^{50}$ Fe | 7/2−# | | |
| $^{51}$ Ni | 28 | 23 | 50.98749(54)# | 23.8(2) ms | β$^+$ (12.3%) | $^{51}$ Co | 7/2−# | | |
| $^{51}$ Ni | 28 | 23 | 50.98749(54)# | 23.8(2) ms | β$^+$, 2p (0.5%) | $^{49}$ Mn | 7/2−# | | |
| $^{52}$ Ni | 28 | 24 | 51.975781(89) | 41.8(10) ms | β$^+$ (68.9%) | $^{52}$ Co | 0+ | | |
| $^{52}$ Ni | 28 | 24 | 51.975781(89) | 41.8(10) ms | β$^+$, p (31.1%) | $^{51}$ Fe | 0+ | | |
| $^{53}$ Ni | 28 | 25 | 52.968190(27) | 55.2(7) ms | β$^+$ (77.3%) | $^{53}$ Co | (7/2−) | | |
| $^{53}$ Ni | 28 | 25 | 52.968190(27) | 55.2(7) ms | β$^+$, p (22.7%) | $^{52}$ Fe | (7/2−) | | |
| $^{54}$ Ni | 28 | 26 | 53.9578330(50) | 114.1(3) ms | β$^+$ | $^{54}$ Co | 0+ | | |
| $^{54}$ Ni | 28 | 26 | 53.9578330(50) | 114.1(3) ms | β$^+$, p? | $^{53}$ Fe | 0+ | | |
| $^{54m}$ Ni | 6457.4(9) keV | 6457.4(9) keV | 6457.4(9) keV | 152(4) ns | IT (64%) | $^{54}$ Ni | 10+ | | |
| $^{54m}$ Ni | 6457.4(9) keV | 6457.4(9) keV | 6457.4(9) keV | 152(4) ns | p (36%) | $^{53}$ Co | 10+ | | |
| $^{55}$ Ni | 28 | 27 | 54.95132985(76) | 203.9(13) ms | β$^+$ | $^{55}$ Co | 7/2− | | |
| $^{56}$ Ni | 28 | 28 | 55.94212776(43) | 6.075(10) d | EC | $^{56}$ Co | 0+ | | |
| $^{56}$ Ni | 28 | 28 | 55.94212776(43) | 6.075(10) d | β$^+$ (<5.8×10$^{−5}$%) | $^{56}$ Co | 0+ | | |
| $^{57}$ Ni | 28 | 29 | 56.93979139(61) | 35.60(6) h | β$^+$ | $^{57}$ Co | 3/2− | | |
| $^{58}$ Ni | 28 | 30 | 57.93534165(37) | Observationally stable | Observationally stable | Observationally stable | 0+ | 0.680769(190) | |
| $^{59}$ Ni | 28 | 31 | 58.93434544(38) | 8.1(5)×10$^4$ y | EC (99%) | $^{59}$ Co | 3/2− | | |
| $^{59}$ Ni | 28 | 31 | 58.93434544(38) | 8.1(5)×10$^4$ y | β$^+$ (1.5×10$^{−5}$%) | $^{59}$ Co | 3/2− | | |
| $^{60}$ Ni | 28 | 32 | 59.93078513(38) | Stable | Stable | Stable | 0+ | 0.262231(150) | |
| $^{61}$ Ni | 28 | 33 | 60.93105482(38) | Stable | Stable | Stable | 3/2− | 0.011399(13) | |
| $^{62}$ Ni | 28 | 34 | 61.92834475(46) | Stable | Stable | Stable | 0+ | 0.036345(40) | |
| $^{63}$ Ni | 28 | 35 | 62.92966902(46) | 101.2(15) y | β$^−$ | $^{63}$ Cu | 1/2− | | |
| $^{63m}$ Ni | 87.15(11) keV | 87.15(11) keV | 87.15(11) keV | 1.67(3) μs | IT | $^{63}$Ni | 5/2− | | |
| $^{64}$ Ni | 28 | 36 | 63.92796623(50) | Stable | Stable | Stable | 0+ | 0.009256(19) | |
| $^{65}$ Ni | 28 | 37 | 64.93008459(52) | 2.5175(5) h | β$^−$ | $^{65}$ Cu | 5/2− | | |
| $^{65m}$ Ni | 63.37(5) keV | 63.37(5) keV | 63.37(5) keV | 69(3) μs | IT | $^{65}$Ni | 1/2− | | |
| $^{66}$ Ni | 28 | 38 | 65.9291393(15) | 54.6(3) h | β$^−$ | $^{66}$ Cu | 0+ | | |
| $^{67}$ Ni | 28 | 39 | 66.9315694(31) | 21(1) s | β$^−$ | $^{67}$ Cu | 1/2− | | |
| $^{67m}$ Ni | 1006.6(2) keV | 1006.6(2) keV | 1006.6(2) keV | 13.34(19) μs | IT | $^{67}$ Ni | 9/2+ | | |
| $^{67m}$ Ni | 1006.6(2) keV | 1006.6(2) keV | 1006.6(2) keV | 13.34(19) μs | IT | $^{67}$ Ni | 9/2+ | | |
| $^{68}$ Ni | 28 | 40 | 67.9318688(32) | 29(2) s | β$^−$ | $^{68}$ Cu | 0+ | | |
| $^{68m1}$ Ni | 1603.51(28) keV | 1603.51(28) keV | 1603.51(28) keV | 270(5) ns | IT | $^{68}$Ni | 0+ | | |
| $^{68m2}$ Ni | 2849.1(3) keV | 2849.1(3) keV | 2849.1(3) keV | 850(30) μs | IT | $^{68}$Ni | 5− | | |
| $^{69}$ Ni | 28 | 41 | 68.9356103(40) | 11.4(3) s | β$^−$ | $^{69}$ Cu | (9/2+) | | |
| $^{69m1}$ Ni | 321(2) keV | 321(2) keV | 321(2) keV | 3.5(4) s | β$^−$ | $^{69}$ Cu | (1/2−) | | |
| $^{69m1}$ Ni | 321(2) keV | 321(2) keV | 321(2) keV | 3.5(4) s | IT (<0.01%) | $^{69}$ Ni | (1/2−) | | |
| $^{69m2}$ Ni | 2700.0(10) keV | 2700.0(10) keV | 2700.0(10) keV | 439(3) ns | IT | $^{69}$Ni | (17/2−) | | |
| $^{70}$ Ni | 28 | 42 | 69.9364313(23) | 6.0(3) s | β$^−$ | $^{70}$ Cu | 0+ | | |
| $^{70m}$ Ni | 2860.91(8) keV | 2860.91(8) keV | 2860.91(8) keV | 232(1) ns | IT | $^{70}$Ni | 8+ | | |
| $^{71}$ Ni | 28 | 43 | 70.9405190(24) | 2.56(3) s | β$^−$ | $^{71}$ Cu | (9/2+) | | |
| $^{71m}$ Ni | 499(5) keV | 499(5) keV | 499(5) keV | 2.3(3) s | β$^−$ | $^{71}$Cu | (1/2−) | | |
| $^{72}$ Ni | 28 | 44 | 71.9417859(24) | 1.57(5) s | β$^−$ | $^{72}$ Cu | 0+ | | |
| $^{72}$ Ni | 28 | 44 | 71.9417859(24) | 1.57(5) s | β$^−$, n? | $^{71}$ Cu | 0+ | | |
| $^{73}$ Ni | 28 | 45 | 72.9462067(26) | 840(30) ms | β$^−$ | $^{73}$ Cu | (9/2+) | | |
| $^{73}$ Ni | 28 | 45 | 72.9462067(26) | 840(30) ms | β$^−$, n? | $^{72}$ Cu | (9/2+) | | |
| $^{74}$ Ni | 28 | 46 | 73.9479853(38) | 507.7(46) ms | β$^−$ | $^{74}$ Cu | 0+ | | |
| $^{74}$ Ni | 28 | 46 | 73.9479853(38) | 507.7(46) ms | β$^−$, n? | $^{73}$ Cu | 0+ | | |
| $^{75}$ Ni | 28 | 47 | 74.952704(16) | 331.6(32) ms | β$^−$ (90.0%) | $^{75}$ Cu | 9/2+# | | |
| $^{75}$ Ni | 28 | 47 | 74.952704(16) | 331.6(32) ms | β$^−$, n (10.0%) | $^{74}$ Cu | 9/2+# | | |
| $^{76}$ Ni | 28 | 48 | 75.95471(32)# | 234.6(27) ms | β$^−$ (86.0%) | $^{76}$ Cu | 0+ | | |
| $^{76}$ Ni | 28 | 48 | 75.95471(32)# | 234.6(27) ms | β$^−$, n (14.0%) | $^{75}$ Cu | 0+ | | |
| $^{76m}$ Ni | 2418.0(5) keV | 2418.0(5) keV | 2418.0(5) keV | 547.8(33) ns | IT | $^{76}$Ni | (8+) | | |
| $^{77}$ Ni | 28 | 49 | 76.95990(43)# | 158.9(42) ms | β$^−$ (74%) | $^{77}$ Cu | 9/2+# | | |
| $^{77}$ Ni | 28 | 49 | 76.95990(43)# | 158.9(42) ms | β$^−$, n (26%) | $^{76}$ Cu | 9/2+# | | |
| $^{77}$ Ni | 28 | 49 | 76.95990(43)# | 158.9(42) ms | β$^−$, 2n? | $^{75}$ Cu | 9/2+# | | |
| $^{78}$ Ni | 28 | 50 | 77.96256(43)# | 122.2(51) ms | β$^−$ | $^{78}$ Cu | 0+ | | |
| $^{78}$ Ni | 28 | 50 | 77.96256(43)# | 122.2(51) ms | β$^−$, n? | $^{77}$ Cu | 0+ | | |
| $^{78}$ Ni | 28 | 50 | 77.96256(43)# | 122.2(51) ms | β$^−$, 2n? | $^{76}$ Cu | 0+ | | |
| $^{79}$ Ni | 28 | 51 | 78.96977(54)# | 44(8) ms | β$^−$ | $^{79}$ Cu | 5/2+# | | |
| $^{79}$ Ni | 28 | 51 | 78.96977(54)# | 44(8) ms | β$^−$, n? | $^{78}$ Cu | 5/2+# | | |
| $^{79}$ Ni | 28 | 51 | 78.96977(54)# | 44(8) ms | β$^−$, 2n? | $^{77}$ Cu | 5/2+# | | |
| $^{80}$ Ni | 28 | 52 | 79.97505(64)# | 30(22) ms | β$^−$ | $^{80}$ Cu | 0+ | | |
| $^{80}$ Ni | 28 | 52 | 79.97505(64)# | 30(22) ms | β$^−$, n? | $^{79}$ Cu | 0+ | | |
| $^{80}$ Ni | 28 | 52 | 79.97505(64)# | 30(22) ms | β$^−$, 2n? | $^{78}$ Cu | 0+ | | |
| $^{81}$ Ni | 28 | 53 | 80.98273(75)# | 30# ms [>410 ns] | β$^−$? | $^{81}$ Cu | 3/2+# | | |
| $^{82}$ Ni | 28 | 54 | 81.98849(86)# | 16# ms [>410 ns] | β$^−$? | $^{82}$ Cu | 0+ | | |
| This table header & footer: view ||||||||||
* ↑ $^m$Ni – 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).
* 1 2 # – 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
* ↑ Bold symbol as daughter – Daughter product is stable.
* ↑ ( ) spin value – Indicates spin with weak assignment arguments.
* ↑ Believed to decay by β$^+$β$^+$ to $^{58}$ Fe with a half-life over 7×10$^{20}$ years
* ↑ Highest binding energy per nucleon of all nuclides

## Notable isotopes

The known isotopes of nickel range in mass number from $^{48}$ Ni to $^{82}$ Ni , and include:
Nickel-48, discovered in 1999, is the most neutron-poor nickel isotope known. With 28 protons and 20 neutrons $^{48}$ Ni is "doubly magic" (like $^{208}$ Pb ) and therefore much more stable (with a lower limit of its half-life-time of .5 μs) than would be expected from its position in the chart of nuclides. It has the highest ratio of protons to neutrons (proton excess) of any known doubly magic nuclide.
Nickel-56 is produced in large quantities in supernovae. In the last phases of stellar evolution of very large stars, nuclear fusion of lighter elements like hydrogen and helium comes to an end. Later in the star's life cycle, elements including magnesium, silicon, and sulfur are fused to form heavier elements. Once the last nuclear fusion reactions cease, the star collapses to produce a supernova. During the supernova, silicon burning produces $^{56}$Ni. This isotope of nickel is favored because it has an equal number of neutrons and protons, making it readily produced by fusing two $^{28}$Si atoms. $^{56}$Ni is the final element that can be formed in the alpha process. Past $^{56}$Ni, nuclear reactions would be endoergic and would be energetically unfavorable. Once $^{56}$Ni is formed it subsequently decays to $^{56}$Co and then $^{56}$Fe by β+ decay. The radioactive decay of $^{56}$Ni and $^{56}$Co supplies much of the energy for the light curves observed for stellar supernovae. The shape of the light curve of these supernovae display characteristic timescales corresponding to the decay of $^{56}$Ni to $^{56}$Co and then to Fe.
Nickel-58 is the most abundant isotope of nickel, making up 68.077% of the natural abundance. Possible sources include electron capture from copper-58 and EC + p from zinc-59.
Nickel-59 is a long-lived cosmogenic radionuclide with a half-life of 81,000 years. $^{59}$ Ni has found many applications in isotope geology. $^{59}$ Ni has been used to date the terrestrial age of meteorites and to determine abundances of extraterrestrial dust in ice and sediment.
Nickel-60 is the daughter product of the extinct radionuclide $^{60}$ Fe (half-life = 2.6 My). Because $^{60}$ Fe had such a long half-life, its persistence in materials in the Solar System at high enough concentrations may have generated observable variations in the isotopic composition of $^{60}$ Ni . Therefore, the abundance of $^{60}$ Ni present in extraterrestrial material may provide insight into the origin of the Solar System and its early history/very early history. Unfortunately, nickel isotopes appear to have been heterogeneously distributed in the early Solar System. Therefore, so far, no actual age information has been attained from $^{60}$ Ni excesses. $^{60}$ Ni is also the stable end-product of the decay of $^{60}$ Zn , the product of the final rung of the alpha ladder. Other sources may also include beta decay from cobalt-60 and electron capture from copper-60.
Nickel-61 is the only stable isotope of nickel with a nuclear spin (I = 3/2), which makes it useful for studies by EPR spectroscopy.
Nickel-62 has the highest binding energy per nucleon of any isotope for any element, when including the electron shell in the calculation. More energy is released forming this isotope than any other, although fusion can form heavier isotopes. For instance, two $^{40}$ Ca atoms can fuse to form $^{80}$ Kr plus 4 positrons (plus 4 neutrinos), liberating 77 keV per nucleon, but reactions leading to the iron/nickel region are more probable as they release more energy per baryon.
Nickel-63 has two main uses: Detection of explosives traces, and in certain kinds of electronic devices, such as gas discharge tubes used as surge protectors. A surge protector is a device that protects sensitive electronic equipment like computers from sudden changes in the electric current flowing into them. It is also used in Electron capture detector in gas chromatography for the detection mainly of halogens. It is proposed to be used for miniature betavoltaic generators for pacemakers.
Nickel-64 is another stable isotope of nickel. Possible sources include beta decay from cobalt-64, and electron capture from copper-64.
Nickel-78 is one of the element's heaviest known isotopes. With 28 protons and 50 neutrons, nickel-78 is doubly magic, resulting in much greater nuclear binding energy and stability despite having a lopsided neutron-proton ratio. It has a half-life of 122 ± 5.1 milliseconds. As a consequence of its magic neutron number, nickel-78 is believed to have an important involvement in supernova nucleosynthesis of elements heavier than iron. $^{78}$Ni, along with N = 50 isotones $^{79}$Cu and $^{80}$Zn, are thought to constitute a waiting point in the r-process, where further neutron capture is delayed by the shell gap and a buildup of isotopes around A = 80 results.