Iron-56

Iron-56, ^56Fe

General
Symbol	^56Fe
Names	iron-56, 56Fe, Fe-56
Protons (Z)	26
Neutrons (N)	30
Nuclide data
Natural abundance	91.754%
Isotope mass	55.9349375(7) Da
Spin	0+
Excess energy	−60601.003±1.354 keV
Binding energy	492253.892±1.356 keV
Isotopes of iron Complete table of nuclides

Nuclear binding energy per nucleon of common isotopes; iron-56 labelled at the curve's crest. The rarer isotopes nickel-62 and iron-58, which both have higher binding energies, are not shown.

Iron-56 (^56Fe) is the most common isotope of iron. About 91.754% of all iron is iron-56.

Of all nuclides, iron-56 has the lowest mass per nucleon. With 8.8 MeV binding energy per nucleon, iron-56 is one of the most tightly bound nuclei.[1]

The high nuclear binding energy for ^56Fe represents the point where further nuclear reactions become energetically unfavorable. Because of this, it is among the heaviest elements formed in stellar nucleosynthesis reactions in massive stars. These reactions fuse lighter elements like magnesium, silicon, and sulfur to form heavier elements. Among the heavier elements formed is ^56Ni, which subsequently decays to ^56Co and then ^56Fe.

Relationship to nickel-62

Nickel-62, a relatively rare isotope of nickel, has a higher nuclear binding energy per nucleon; this is consistent with having a higher mass-per-nucleon because nickel-62 has a greater proportion of neutrons, which are slightly more massive than protons. (See the nickel-62 article for more). Light elements undergoing nuclear fusion and heavy elements undergoing nuclear fission release energy as their nucleons bind more tightly, so ^62Ni might be expected to be common. However, during stellar nucleosynthesis the competition between photodisintegration and alpha capturing causes more ^56Ni to be produced than ^62Ni (^56Fe is produced later in the star's ejection shell as ^56Ni decays).

Although nickel-62 has a higher binding energy per nucleon, the conversion of 28 atoms of nickel-62 into 31 atoms of iron-56 releases 0.011 Da of energy. As the universe ages, matter will slowly convert to ever more tightly bound nuclei, approaching ^56Fe, ultimately leading to the formation of iron stars over ≈ 10^1500 years, assuming an expanding universe without proton decay.[2]

See also

• Isotopes of iron
• Iron star

References

1. Nuclear Binding Energy
2. Dyson, Freeman J. (1979). "Time without end: Physics and biology in an open universe". Reviews of Modern Physics. 51 (3): 447–460. Bibcode:1979RvMP...51..447D. doi:10.1103/RevModPhys.51.447.

• de Laeter, John Robert; Böhlke, John Karl; De Bièvre, Paul; Hidaka, Hiroshi; Peiser, H. Steffen; Rosman, Kevin J. R.; Taylor, Philip D. P. (2003). "Atomic weights of the elements. Review 2000 (IUPAC Technical Report)". Pure and Applied Chemistry. 75 (6): 683–800. doi:10.1351/pac200375060683.

Lighter: iron-55	Iron-56 is an isotope of iron	Heavier: iron-57
Decay product of: manganese-56 cobalt-56	Decay chain of iron-56	Decays to: Stable