Hafnium–tungsten dating is a geochronological radiometric dating method utilizing the radioactive decay system of hafnium-182 to tungsten-182. The half-life of the system is 8.9±0.1 million years. Today hafnium-182 is an extinct radionuclide, but the hafnium–tungsten radioactive system is useful in studies of the early Solar System since hafnium is lithophilic while tungsten is moderately siderophilic, which allows the system to be used to date the differentiation of a planet's core. It is also useful in determining the formation times of the parent bodies of iron meteorites. The use of the hafnium-tungsten system as a chronometer for the early Solar System was suggested in the 1980s, but did not come into widespread use until the mid-1990s when the development of multi-collector inductively coupled plasma mass spectrometry enabled the use of samples with low concentrations of tungsten.
Basic principle The radioactive system behind hafnium–tungsten dating is a two-stage decay as follows:
18272Hf → 18273Ta + e− + νe 18273Ta → 18274W + e− + νe The first decay has a half-life of 8.9 million years, while the second has a half-life of only 114 days, such that the intermediate nuclide tantalum-182 (182Ta) can effectively be ignored. Since hafnium-182 is an extinct radionuclide, hafnium–tungsten chronometry is performed by examining the abundance of tungsten-182 relative to other stable isotopes of tungsten, of which there are effectively five in total, including the extremely long-lived isotope tungsten-180, which has a half-life much longer than the current age of the universe. The abundance of tungsten-182 can be influenced by processes other than the decay of hafnium-182, but the existence of a large number of stable isotopes is very helpful for disentangling variations in tungsten-182 due to a different cause. For example, while 182W, 183W, 184W and 186W are all produced by the r- and s-processes, the rare isotope tungsten-180 is only produced by the p-process. Variations in tungsten isotopes caused by r- and s-process nucleosynthetic contributions also result in correlated changes in the ratios 182W/184W and 183W/184W, which means that the 183W/184W ratio can be used to quantify how much of the tungsten-182 variation is due to nucleosynthetic contributions. The influence of cosmic rays is more difficult to correct for since cosmic ray interactions affect the abundance of tungsten-182 much more than any of the other tungsten isotopes. Nonetheless, cosmic ray effects can be corrected for by examining other isotope systems such as platinum, osmium or the stable isotopes of hafnium, or simply by taking samples from the interior that have not been exposed to cosmic rays, though the latter requires large samples. Tungsten isotopic data is usually plotted in terms of ε182W and ε183W, which represent deviations in the ratios 182W/184W and 183W/184W in parts per 10,000 relative to terrestrial standards. Since Earth is differentiated the crust and mantle of Earth are enriched in tungsten-182 relative to the initial composition of the Solar System. Undifferentiated chondritic meteorites have ε182W = −1.9±0.1 relative to Earth, which is extrapolated to give a value of −3.45±0.25 for the initial ε182W of the Solar System.
Dating planetary core formation A primordial planet is undifferentiated, meaning that it is not layered according to density (with the densest material being towards the interior of the planet). When a planet undergoes differentiation the dense materials, particularly iron, separate from lighter components and sink to the interior forming the core of the planet. If this process took place relatively early in a planet's history, hafnium-182 would not have sufficient time to decay to tungsten-182. Since hafnium is a lithophile element the (undecayed) hafnium-182 would remain in the mantle (i.e. the outer layers of the planet). Then, after some time, the hafnium-182 would decay to tungsten-182 leaving an excess of tungsten-182 in the mantle. On the other hand, if differentiation occurred later in a planet's history, then most of the hafnium-182 would have decayed to tungsten-182 before differentiation began. Being moderately siderophilic, much of the tungsten-182 would sink towards the interior of the planet along with iron. In this scenario, not much tungsten-182 would subsequently be present in the outer layers of the planet. As such, by looking at how much tungsten-182 is present in the outer layers of a planet, relative to other isotopes of tungsten, the time of differentiation can be quantified.
Model ages If we have a sample from the mantle (or core) of a body and want to calculate a core formation age from the tungsten-182 abundance we need to also know the composition of the bulk planet. Since we do not have samples from the core of Earth (or any other intact planet) the composition of chondritic meteorites is generally substituted for that of the bulk planet. Hafnium and tungsten are both refractory elements so there is not expected to be any fractionation between hafnium and tungsten due to heating of the planet during or after formation. A model age for the time of core formation can then be calculated using the equation
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