Isotopes of iron

Natural iron consists of four stable isotopes: 5.85% Fe, 91.75% Fe, 2.12% Fe and 0.28% Fe. There are 28 known radioisotopes and 8 nuclear isomers, the most stable of which are Fe and Fe.
Much of the past work on measuring the isotopic composition of iron has centered on determining Fe variations due to processes accompanying nucleosynthesis and ore formation. In the last decade however, advances in mass spectrometry technology have allowed the detection and quantification of minute, naturally occurring variations in the ratios of the stable isotopes of iron. Much of this work has been driven by the Earth and planetary science communities, though applications to biological and industrial systems are beginning to emerge.

List of isotopes

Iron-56

Fe is the most abundant isotope of iron. It is also the isotope with the lowest mass per nucleon, 930.412 MeV/c, though not the isotope with the highest nuclear binding energy per nucleon, which is nickel-62. However, because of the details of how nucleosynthesis works, Fe is a more common endpoint of fusion inside supernovae, where it is mostly produced as Ni, which subsequently decays to Co and then iron. Thus, Fe is more common in the universe, relative to other heavy elements, including Ni, Fe, and Ni, all of which have a comparably high binding energy.

Iron-57

Fe is widely used in Mössbauer spectroscopy and the related nuclear resonance vibrational spectroscopy due to the low natural variation in energy of the 14.4 keV nuclear transition.
The transition was famously used to make the first definitive measurement of gravitational redshift, in the 1960 Pound–Rebka experiment.

Iron-60

Iron-60 has a half-life of 2.62 million years, but was thought until 2009 to have a half-life of 1.5 million years. It undergoes beta decay to ⁶⁰Co, which then decays with the much shorter half-life of about 5 years to stable ⁶⁰Ni.
In phases of the meteorites Semarkona and Chervony Kut, a correlation between the excess concentration of Ni, the granddaughter isotope of Fe, and the abundance of the stable iron isotopes could be found, which is evidence for the existence of Fe at the time of formation of the Solar System. Depending on its original abundance, the energy from the decay of Fe may have been significant, along with that of Al, to the remelting and differentiation of asteroids and planetesimals after their formation. These nickel abundances in extraterrestrial materials may also provide further insight into the origin of the Solar System and its early history.
Live iron-60 was first identified in deep sea sediments in 1999. These are deep sea ferromanganese crusts, which are constantly growing, aggregating iron, manganese, and other elements. Iron-60 has been found in fossilized bacteria in sea floor sediments. In 2019, researchers found Fe in Antarctica. 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 the Local Bubble and likely the Orion–Eridanus Superbubble. These superbubbles were created by multiple supernovae. 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 4πr. The fraction of the material intercepted by the Earth is dependent on its cross-sectional area as it passes through the expanding debris:
where M is the mass of ejected material. Assuming the intercepted material is distributed uniformly across the surface of the Earth, the mass surface density of the supernova ejecta on Earth is:
The number of Fe atoms per unit area found on Earth can be estimated if the typical amount of Fe ejected from a supernova is known. This can be done by dividing the surface mass density by the atomic mass of Fe.
The equation for N can be rearranged to find the distance to the supernova.
An example calculation for the distance to the supernova point of origin is given below. This calculation uses speculative values for terrestrial Fe atom surface density and a rough estimate of the mass of Fe ejected by a supernova.
More sophisticated analyses have been reported that take into consideration the flux and deposition of Fe as well as possible interfering background sources.
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 for gamma-ray astronomy, and have been detected by the gamma-ray observatory INTEGRAL. The signal traces the Galactic plane, showing that Fe synthesis is ongoing in our galaxy, and probing element production in massive stars.