Skip to main content

Thank you for visiting You are using a browser version with limited support for CSS. To obtain the best experience, we recommend you use a more up to date browser (or turn off compatibility mode in Internet Explorer). In the meantime, to ensure continued support, we are displaying the site without styles and JavaScript.

Experimental evidence for hydrogen incorporation into Earth’s core


Hydrogen is one of the possible alloying elements in the Earth’s core, but its siderophile (iron-loving) nature is debated. Here we experimentally examined the partitioning of hydrogen between molten iron and silicate melt at 30–60 gigapascals and 3100–4600 kelvin. We find that hydrogen has a metal/silicate partition coefficient DH ≥ 29 and is therefore strongly siderophile at conditions of core formation. Unless water was delivered only in the final stage of accretion, core formation scenarios suggest that 0.3–0.6 wt% H was incorporated into the core, leaving a relatively small residual H2O concentration in silicates. This amount of H explains 30–60% of the density deficit and sound velocity excess of the outer core relative to pure iron. Our results also suggest that hydrogen may be an important constituent in the metallic cores of any terrestrial planet or moon having a mass in excess of ~10% of the Earth.


Existing Earth’s core formation models constrained by partitioning of moderately siderophile elements suggest that metals equilibrated with molten silicates in a deep “magma ocean” under high-pressure and -temperature (P–T) conditions up to about 60 GPa and 4000 K1,2,3,4,5,6 (Supplementary Fig. 1). While hydrogen is one of the plausible impurity elements in the iron-rich core7, its metal–silicate partitioning under such conditions has been controversial in both experiments8,9,10,11,12 and theory13,14,15. Previous experimental studies on the metal–silicate partitioning of hydrogen were performed below 20 GPa using molten8,11,12 and solid9,10 silicates. While hydrogen has been found to be strongly siderophile under high pressure8,9,10, these results were challenged by more recent experiments11,12. These later studies11,12 found low hydrogen concentrations in iron, which may be attributed to the fact that they conducted carbon-saturated experiments, leading to carbon enrichment in metal that may hinder hydrogen incorporation. It is also possible that hydrogen escaped from their samples prior to measurements performed after they were decompressed and recovered at ambient conditions, where FeHX is known to decompose10 into bcc Fe and molecular H2. The equilibrium hydrogen solubility in bcc Fe at an H2 pressure of 1 bar is limited to16 X  < 10−5. Loss of hydrogen from iron samples during decompression has been demonstrated in previous neutron diffraction10 as well as our new X-ray diffraction (XRD) measurements (Supplementary Fig. 2).

Here, we report experiments to constrain the partitioning of hydrogen between molten iron and silicate melt at high P–T to 60 GPa. The results demonstrate the strongly siderophile nature of hydrogen under conditions where metals segregated from silicates during Earth’s core formation, suggesting that hydrogen is an important light element in the core. In addition, hydrogen may be a major impurity element in the metallic cores of other terrestrial planets and moons whose masses are more than 10% of that of the Earth.

Results and discussion

Metal–silicate partitioning of hydrogen

We carried out metal–silicate partitioning experiments at 30–60 GPa and 3100–4600 K in a diamond-anvil cell (DAC) (Supplementary Table 1 and Supplementary Fig. 3) and found 5300 to 26,000 ppm H (by weight) in metal at high pressure (before decompression), on the basis of the phase proportion and lattice volume of FeHX and ε-FeOOH that formed from liquid iron upon temperature quenching under sustained confining pressure (Fig. 1a) (see “Methods”). Note that liquid iron was likely to have quenched fully to crystals and subsequent thermal annealing in a separate experiment had a negligible effect upon hydrogen concentrations (only 6% difference)17. On the other hand, we obtained 90–470 ppm H (present as H2O) in quenched silicate melts by measuring recovered samples using a high-resolution imaging technique coupled with secondary ion mass spectrometry (SIMS) (Fig. 1b), which enabled quantitative compositional analysis of a small DAC sample (see “Methods”). In \(D_{\mathrm{H}}^{{\mathrm{metal/silicate}}}\) we found ranges from 29 to 57 by weight (Fig. 2a), indicating that hydrogen is siderophile at these P–T conditions.

Fig. 1: Analyses of hydrogen in metal and silicate.
figure 1

a XRD patterns collected before/during/after heating to 3920 K at 46 GPa in run #1. Both iron and silicate were molten at the center of a laser-heated spot during heating. Hydrogen concentration in liquid metal was obtained from those in fcc FeHX and ε-FeOOH. b Photomicrograph (left), secondary ion images for 1H+, 28Si+, and 40Ca+ (middle), and a distribution map of water (right). Note the absence of hydrogen in metal because it escaped from iron upon releasing pressure. Hydrogen (water) content in quenched silicate melt was obtained with ±2% to ±7% relative uncertainty.

Fig. 2: Metal–silicate partitioning of hydrogen.
figure 2

a Partition coefficient D (by weight) for hydrogen as a function of reciprocal temperature. The present experiments (red circles) show that hydrogen is strongly siderophile under conditions of Earth’s core formation. Recent experimental studies (gray diamonds11, orange squares12) reported D values lower by one to three orders of magnitude than the present results, which is likely attributed to hydrogen loss from metals during decompression. Pioneer experimental results8 (blue inverted triangles) and recent theoretical values (star13, pink crosses15, and blue pluses14 for H and green pluses14 for H2O; large and small symbols indicate maximum and minimum values, respectively) are also plotted. b Exchange coefficient KD for Eq. 2. The numbers given to each datum point and regression line indicate pressure conditions.

The metal–silicate partitioning of hydrogen can be expressed as a chemical reaction,

$${\mathrm{HO}}_{0.5}^{{\mathrm{silicate}}\,{\mathrm{melt}}} + \frac{1}{2}{\mathrm{Fe}}^{{\mathrm{metal}}} = {\mathrm{H}}^{{\mathrm{metal}}} + \frac{1}{2}{\mathrm{FeO}}^{{\mathrm{silicate{\kern 1pt}} melt}}$$

The exchange coefficient KD is parameterized as a function of P (GPa) and T(K) with regression constants a, b, and c (Fig. 2b),

$$\begin{array}{*{20}{l}}\log _{10}K_{\mathrm{D}}\hfill & \!\!\! =\ \hfill & {\mathrm{log}}_{10}\frac{{x_{\mathrm{H}}^{\prime{\mathrm{metal}}}}}{{x_{{\mathrm{HO}}_{0.5}}^{{\mathrm{silicate}}}}} \cdot \sqrt {\frac{{x_{{\mathrm{FeO}}}^{{\mathrm{silicate}}}}}{{x_{{\mathrm{Fe}}}^{\prime{\mathrm{metal}}}}}}\hfill\\ \hfill& \!\!\!=\!\!\! \hfill & {\mathrm{log}}_{10}\frac{{x_{\mathrm{H}}^{\prime{\mathrm{metal}}}}}{{x_{{\mathrm{HO}}_{0.5}}^{{\mathrm{silicate}}}}} + \frac{1}{4}\Delta {\mathrm{IW}}\\ & \!\!\!=\!\!\! \hfill & a + \frac{b}{T} + c \cdot \frac{P}{T}\hfill\end{array}$$

where x represents molar fraction (see “Methods” for x′) and the effects of Si, O, and C are not parameterized explicitly. Oxygen fugacity fO2 relative to the iron-wüstite (IW) buffer is approximated as \(\Delta {\mathrm{IW}} \approx 2\log _{10}\left( {x_{{\mathrm{FeO}}}^{{\mathrm{silicate}}}/x _{{\mathrm{Fe}}}^{\prime{\mathrm{metal}}}} \right)\) following previous studies2,3. Least-squares fitting to our data yields a = 2.42 (18), b = −2892 (433), and c = −32.0 (87).

Incorporation of hydrogen during core formation

The partition coefficient only constrains the relative proportion of hydrogen in metal and silicates at equilibrium. In order to estimate the amount of hydrogen that entered metal during core formation, it is necessary to specify the concentration of H2O in the silicate magma ocean (MO) with which it equilibrated. If we assume that negligible hydrogen is able to enter the core after formation, and that hydrogen was continuously delivered to the proto-Earth during accretion (as opposed to late), then plausible estimates of the residual amount in the present-day mantle (291 ppm)18, crust, oceans, and atmosphere (1.6 × 1024 g)19, altogether comprising the bulk silicate Earth (BSE) during accretion, gives a value of 687 ppm H2O. If the Earth lost 0.1–1 ocean mass of water20,21 (OC) by escape of hydrogen to space, this estimate would be considered a lower bound for H2O concentrations prevailing in the MO. Acknowledging the many uncertainties in this estimate, we will use 687 ppm H2O in the proto-Earth BSE (Fig. 3) in order to examine how much hydrogen could plausibly have been incorporated into the Earth’s core.

Fig. 3: Estimate of hydrogen concentration in the core based on single-stage core formation models.
figure 3

Three solid lines show our estimates of the hydrogen content in the core as a function of residual H2O abundance in silicates (= present-day BSE water content) at the labeled P–T conditions2,3,4. The BSE water content depends largely on the average mantle abundance (lower horizontal axis)18,64,65. Even a modest amount of water in the present-day mantle18 and resulting 687 ppm H2O in the BSE suggest 0.32–0.61 wt% H in the core. The corresponding ocean mass of water (OC) that includes an equivalent amount of hydrogen is also indicated (right vertical axis).

We calculated the amount of hydrogen that would be incorporated from silicates into metals based on three different core formation models. First we considered a conceptually simple, single-stage core formation model2,3,4 (see “Methods”), which reconciles the mantle abundances of moderately siderophile elements with entire core–mantle chemical equilibration taking place at a single P, T, and fO2 condition, around 50 GPa and 3500 K (Supplementary Fig. 1) and ΔIW = −2.3. While such a model is physically unrealistic, it is nevertheless useful as a simple reference for comparison. With these assumptions, we estimate that a core forged under this scenario would contain 0.32–0.61 wt% H in equilibrium with molten silicate containing 687 ppm H2O (Fig. 3 and Supplementary Table 2).

Next we examined a continuous core formation model5 (Supplementary Fig. 4) in which core segregation occurred over 1000 accretion events and the impactor core equilibrated with the entire MO at P–T conditions prevailing at its base (see “Methods”). We followed a specific model (path 6) given by Badro et al.5 for the evolution of fO2 in metal–silicate equilibration. Considering three different water delivery scenarios, we find that 0.3–0.6 wt% H in the core is necessary to leave a residual budget of ~690 ppm H2O in the BSE unless water was delivered only in the last stage of Earth accretion.

We also applied a multi-stage core formation model6 (Fig. 4 and Supplementary Fig. 5), where metal–silicate partitioning took place by 1000 steps upon accretion of identical impactors having the same water abundance and the metal from each impactor equilibrated only with a limited fraction of silicate melt at the base of the existing MO (see “Methods”). In this model, fO2 is given as a consequence of the metal–silicate partitioning of H, Ni, Co, O, and Si. We have explored reasonable sets of parameters—impactor size, final (maximum) P at the bottom of the MO, impactor’s metal/oxide proportions of Fe and Si, and H2O concentration (Supplementary Fig. 6 and Supplementary Table 3), which allow for a remaining ~700 ppm H2O in the BSE and yielding the correct core mass and mantle FeO, Ni and Co abundances. These accretion models imply that the core includes 0.27–0.56 wt% H after accretion (Supplementary Table 4).

Fig. 4: Evolutions during multi-stage core formation.
figure 4

a P and T and b fO2 conditions for metal–silicate equilibrium. c Core mass fraction. FeO (d), Ni (e), Co (f), and H2O (h) in the silicate; and O and Si (g) and H (i) in the core. Each model, S1 (red), F2 (black), and R3 (purple) in Supplementary Table 4, employed a different combination of P–T path (a) and partitioning data2,3,6,57,63 for elements other than hydrogen (see Supplementary Table 3 for each parameter set). The present Earth values are shown by gray bands.

In summary, our new experimental determination of metal–silicate partitioning of hydrogen suggests 0.3–0.6 wt% H was incorporated into the core, leaving ~700 ppm H2O in a magma ocean, unless water was delivered only in the late stage of Earth accretion22. We would find more hydrogen in the core if magma oceans contained more water (Fig. 3). According to theoretical calculations23,24, a hydrogen-rich outer core is compatible with seismological observations, with 0.3–0.6 wt% H accounting for 30–60% of the density deficit and sound velocity excess of the outer core. A value of 0.3–0.6 wt% H in the core is equivalent to the amount of hydrogen in 37–73 OCs (Fig. 3), and an additional ~2 OCs are included in our assumed BSE (including the ocean itself). Such a large amount of water, corresponding to 0.9–1.7% Earth’s mass, must have been delivered to our planet during accretion. The core is expected to have a lower D/H than equilibrated silicates25, some of which may have leaked into the mantle26 along with other core-like isotopic signatures27. The delivery of a few tens to hundreds times OCs to the growing Earth is supported by some recent planet formation scenarios28,29,30. In addition, any terrestrial planets and moons greater than ~10% of the Earth’s mass may contain >0.15 wt% H in their metallic cores (Supplementary Fig. 5i) if they formed under conditions similar to that of Earth’s formation and water was continuously supplied during accretion.


Starting materials

We used pure iron foil (5N, Mairon-UHP, Toho Zinc Co. Ltd.) and hydrous MORB glass as starting materials. MORB glasses containing about 0.2 and 1.0 wt% H2O were synthesized using a piston-cylinder apparatus. The major element composition is similar to the one employed in previous experimental studies31,32 (Supplementary Table 5). Water content in the glass was confirmed using SIMS analyses (see below).

High-pressure and -temperature experiments

Experiments were performed in a laser-heated DAC with flat 300 μm culet diamond anvils. Iron foil (5–7 μm thick) was sandwiched between the hydrous MORB glass powder and loaded into a ~140 µm hole at the center of a pre-indented rhenium gasket. We used the MORB glass with ~1.0 wt% H2O, except for run #1 in which ~0.6 wt% H2O was added by mixing glass containing 0.2 and 1.0 wt% H2O. After loading the sample, the entire DAC was dried in a vacuum oven at 400 K for 3–8 h. As soon as the DAC was taken out of the oven, we immediately started compression.

The sample was heated at high pressure while collecting in situ XRD data at beamline BL10XU, SPring-8. Heating was applied from both sides using two 100 W single-mode Yb fiber lasers (SPI photonics). The laser beam was converted to a flat-top distribution using beam shaping optics (New Focus). The laser spot size was around 40 μm. Heating duration was limited to 3 s to avoid temperature fluctuations that could give rise to complex melting textures. This is sufficient time for each element to diffuse in liquid metal33 and silicate34. Earlier time-series experiments32 on element partitioning in a DAC also showed that partition coefficients did not change after heating for 1–2 s. Temperature was measured using a spectro-radiometric method, and a one-dimensional radial temperature profile was obtained across a laser-heated spot with 1 μm spatial resolution. Experimental temperature was estimated by averaging over the 6 μm span of the X-ray beam. Temperature uncertainty35 may be ±5%. Sample pressure was determined from the Raman shift of the diamond anvil36 at ambient temperature after heating. We added an additional contribution of thermal pressure that has been estimated to be +2.5 GPa per 1000 K37 .

In situ XRD measurement and the hydrogen content in metal

XRD patterns were collected before/during/after heating in each run. A monochromatic X-ray beam with an energy of ~30 keV was focused to 6 μm area (full-width at half-maximum) on a sample position. The XRD data were collected every 0.22 s during heating on a flat panel detector (Perkin Elmer) (Fig. 1a).

Since hydrogen escapes from solid iron during decompression as it transforms into bcc Fe10,16 (Supplementary Fig. 2), hydrogen concentration must be measured at high pressure. The XRD patterns demonstrate that molten iron crystallized FeHX and minor FeOOH upon quenching the temperature while maintaining compression (Fig. 1a). The disappearance of a diffuse signal suggests that quenched molten iron fully consisted of crystals even without thermal annealing. Therefore the FeHX + minor FeOOH represents the bulk hydrogen concentration in metal. Hydrogen content in molten iron was therefore determined from (1) the proportions of solid FeHX and FeOOH in quenched liquid iron and (2) the X value in FeHX that is calculated from its unit-cell volume at high pressure (Supplementary Table 1). Earlier experiments have demonstrated that thermal annealing of such FeHX quench crystals had a relatively small effect on their unit-cell volume; hydrogen content X derived from the lattice volume (see below) decreased from 1.21 to 1.14 upon heating to ~1500 K at 65 GPa17.

Here, hcp FeHX>1 and fcc FeHX<1 were formed in run #4 and the other runs, respectively. Since hydrogen incorporation expands the volume of Fe, hydrogen concentration in FeHX can be obtained38 as:

$$X = (V_{{\mathrm{FeH}}_X} - V_{{\mathrm{Fe}}})/\Delta V_{\mathrm{H}}$$

where \(V_{{\mathrm{FeH}}_X}\) is the volume of FeHX per Fe atom and ΔVH is the volume increase per hydrogen atom39, consistent with recent neutron diffraction data40,41. The volume of pure Fe is from Dewaele et al.42 for hcp and from Tsujino et al.43 for fcc. The X value was found to be homogeneous in the metal.

The unit-cell volume of ε-FeOOH was similar to that observed in recent high-pressure studies at equivalent pressure44. Since FeO was not observed, the proportions of FeHX and FeOOH are estimated from the Fe and O contents in quenched liquid iron that were obtained by electron probe micro-analyzer (EPMA) analyses (see below).

SIMS analysis and the hydrogen content in silicate melt

After recovering the DAC sample at ambient conditions, a cross-section at the center of the laser-heated portion was prepared parallel to the compression/laser-heating axis by using a dual-beam focused ion beam (FIB, Versa 3DTM, FEI). Textural observation and preliminary compositional characterization were made with a field-emission-type scanning electron microscope (FE-SEM) and an energy-dispersive X-ray spectrometer (EDS) with a silicon drift detector (Bruker) in the dual-beam FIB system (Supplementary Fig. 3).

Subsequently the hydrogen content in a quenched silicate melt was determined with an isotope microscope system installed at the Hokkaido University, which is composed of CAMECA IMS-1270 SIMS and a two-dimensional ion detector, SCAPS (stacked CMOS-type active pixel sensor)45. This system provides quantitative maps of secondary ions emitted from sample surface46,47 (Fig. 1b), because the CMOS sensor exhibits a good linear relationship between an output voltage and the number of secondary ions48). Therefore, we can quantify the abundance of each element from the intensity map.

Two-dimensional images of 1H+, 28Si+, and 40Ca+ with 0.5–1.2 µm spatial resolution for 1H+ were collected using the 16O primary beam (13 keV, 37 nA) that was focused to 20–30 μm in diameter and rastered across a 100 μm × 100 μm region on the sample surface. We set the contrast aperture to be 100 μm in diameter with the exit slit fully opened. In order to minimize the effect of adsorbed water on the sample surface, we employed the energy slit to be ±20 eV to select kinetic energy ranges of secondary ions from 80 to 120 eV by loading a sample offset voltage of −100 V. The pressure during measurements was 6.5–8.0 × 10−8 Pa. Secondary ion images of 1H+, 28Si+, and 40Ca were obtained sequentially in the following order; 28Si+, 1H+, 28Si+, 1H+, 28Si+, and 40Ca+. Accumulation time was 500 and 100 s in each image, and two and three images were combined to calculate concentration maps for 1H+ and 28Si+, respectively.

Hydrogen concentration in the quenched silicate melt was quantified from the 1H/28Si intensity ratio using a calibration curve established by three silicate glasses with known H2O concentrations (0.00–4.5 wt%)49 (Supplementary Fig. 7). The analyses of these standards provide a linear relation between the count and known 1H/28Si ratios; a correlation coefficient R2 = 0.996. The detection limit of H2O is 15 ppm from its y-intercept. These standards were measured before, during, and after the analysis of each DAC sample. In order to reduce statistical errors for each DAC sample, regions of interest (ROIs) were selected on the quenched silicate melt. Combining the 1H/28Si intensity ratio with the Si content obtained by a field-emission-type electron probe micro-analyzer (FE-EPMA, see below), hydrogen (water) concentration in silicate melt was determined with ±2% to ±7% uncertainty, depending on its abundance (Supplementary Table 1).

Chemical analysis with FE-EPMA

The major element compositions, except hydrogen, of both quenched liquid metal and silicate melt were determined using an FE-EPMA (JXA-8530F, JEOL) (Supplementary Tables 5 and 6). Analyses were performed with an acceleration voltage of 12 keV and a beam current of 15 nA. For metal, we used an electron beam diameter of 3 μm, Fe, Al2O3, Ni2Si, and Mg as standards, and LIFH (Fe), LDE1H (O), PETJ (Si), and TAP (Al, Mg) as analyzing crystals. For silicate, the standards were SiO2, TiO2, Al2O3, Fe2O3, MgO, CaSiO3, NaAlSi3O8, and KAlSi3O8, and the analyzing crystals were TAP (Si, Mg, Na), PETJ (Ti, K), TAPH (Al), LIFH (Fe), and PETH (Ca). We employed the EDS analyses of oxygen and silicon only for run #2, because the metal part was sputtered out during SIMS analyses. In addition, the carbon contents in metal were determined separately without carbon-coating using the LDE2 analyzing crystal and Fe3C as a standard17.

Activities of elements in hydrogen-rich metal and oxygen fugacity

The hydrogen content X in FeHX ranged from 0.23 to 1.78 in the present study (Supplementary Table 1). Large X significantly decreases the molar fractions of Fe and O in metal. And, it apparently increases the oxygen fugacity \(\Delta {\mathrm{IW}} \approx 2\log _{10}\left( {x_{{\mathrm{FeO}}}^{{\mathrm{silicate}}}{\mathrm{/}}x_{{\mathrm{Fe}}}^{{\mathrm{metal}}}} \right)\) and decreases the exchange coefficient \(K_{\mathrm{D}}^{\mathrm{O}} = \frac{{x_{{\mathrm{Fe}}}^{{\mathrm{metal}}}x_{\mathrm{O}}^{{\mathrm{metal}}}}}{{x_{{\mathrm{FeO}}}^{{\mathrm{silicate}}}}}\) for the reaction FeOsilicate = Femetal + Ometal.

We obtain the \(K_{\mathrm{D}}^{\mathrm{O}}\) values from this study using molar fractions of iron and oxygen in metal, with and without considering the presence of hydrogen and carbon. They are compared with the results of Fischer et al.3 that were obtained in the absence of hydrogen and carbon (Supplementary Fig. 8). The present \(K_{\mathrm{D}}^{\mathrm{O}}\) values that do not take hydrogen and carbon into account are closer to their data, suggesting that hydrogen and carbon do not have colligative properties in iron solvent. It is likely because the incorporation of small H and C atoms in liquid Fe is interstitial rather than substitutional unlike other larger atoms23. Therefore, in this study, we approximate the activity of element i in metal as:

$$x_i^\prime = \frac{{N_i}}{{\mathop {\sum}\nolimits_{k \ne {\mathrm{H,C}}} {N_k} }}$$

Note that this formulation has been conventionally used in solid metal-hydrogen systems50. The slope on a plot log10D vs. ΔIW obtained with this formulation indicates a valence state of 0.999 for hydrogen in the silicate melt (Supplementary Fig. 9), which supports the validity of the present estimate of the activities of elements in metal and silicate. Our experiments give log10\(K_{\mathrm{D}}^{\mathrm{O}}\) = a + b/T, where a = 0.37 (18) and b = −1535 (687).

Single-stage core formation model

Single-stage core formation models2,3,4 assume the entire core and mantle equilibrate at a single P, T, and fO2 condition. We employed three different P–T conditions at fixed fO2 (ΔIW = −2.3) that is compatible with the FeO content of the mantle (Supplementary Table 2), which have been proposed on the basis of different sets of partitioning data for siderophile elements2,3,4. The present experiments demonstrate that hydrogen is strongly siderophile under these conditions; the metal/silicate partition coefficient \(D_{\mathrm{H}}^ \ast\) ranges from 38 to 70 (Supplementary Fig. 1) (see its caption for \(D_{\mathrm{H}}^ \ast\) that is defined for simplicity). Previous studies2,3,4 have already calculated the partitioning of O and Si. We assume that the presence of H and H2O does not change the partitioning of siderophile elements51,52, O (Supplementary Fig. 8) and Si.

Our calculations give 0.32–0.61 wt% H in the core when equilibrated with a KLB-1 pyrolitic melt53 containing 687 ppm H2O (Fig. 3). The resulting core also includes 0 (assumed)–2.5 wt% O and 4.5–13.3 wt% Si, in addition to 0.32–0.61 wt% H and likely 2.0 wt% S that is inferred from cosmo-/geochemical arguments54 (Supplementary Table 2). This liquid is less dense than the present outer core24,55, possibly suggesting that it later become depleted in Si + O following SiO2 crystallization56.

Continuous core formation model

The continuous core formation model considers that the Earth accreted incrementally and the metal in each impactor chemically equilibrated with the entire magma ocean (MO). The P–T conditions are assumed to correspond to the base of the MO4,5. While Wade and Wood4 argued that the oxidation state for core segregation was initially reductive and became progressively more oxidative to the current state (ΔIW = −2.3), Badro et al.5 demonstrated that starting with oxidative conditions can better explain the mantle abundances of moderately siderophile elements on the basis of metal–silicate partitioning experiments at higher pressures57.

We performed 1000-step calculations of metal–silicate partitioning of hydrogen at evolving P, T, and fO2 conditions following path 6 in Badro et al.5; for ith step, PMOB,i = Pfinal × (i/1000)2/3 (Pfinal = 62 GPa) and TMOB1,i = 2022 + 54.21PMOB,i − 0.34 \(P_{{\mathrm{MOB}},i}^2\) + 9.0747 × 10−4 \(P_{{\mathrm{MOB}},i}^3\) (K) (Supplementary Fig. 1), which explains the mantle abundances of Ni, Co, V, and Cr as well as FeO. Details are found in Dauphas58. Each impactor possesses 32.5 wt% metal (same as the present-day Earth). Silicate composition is pyrolitic59 except for FeO that is controlled by fO2 in the model. Evolution of the Si and O abundances in the core are shown in Fig. S2 in Badro et al.5. The effects of H2O and H on metal/silicate partitioning of the other elements are not considered (see51,52 and Supplementary Fig. 8). According to Iizuka-Oku et al.10 and Fukai and Suzuki16, no hydrogen is partitioned into metal when PMOB,i < 3 GPa.

Three different scenarios were considered for the delivery of water: (1) constant, (2) linearly increases, and (3) none but the last seven impactors (Supplementary Fig. 4a). For each scenario, we have examined hydrogen concentrations in the core when ~690 ppm H2O remains in the silicate after accretion (Supplementary Fig. 4b). For scenario 1, hydrogen concentration in the core is almost constant at 0.60 wt% during accretion (Supplementary Fig. 4c). While 0.30 wt% H is found in the core with scenario 2, only 25 ppm is present in scenario 3. It is possible that water derives predominantly from a late veneer after core formation22, leading to the minimal incorporation of hydrogen into the core.

Multi-stage core formation model

We also examined the multi-stage core formation model, in which core segregation occurred by multiple steps upon accretional impacts and each time impactor core metal equilibrated with a limited portion of silicate in the existing MO at the P–T condition of its base6,60. While Rubie et al.6 assumed that hydrogen is not siderophile and employed DH = 0.05–0.5, we apply DH > 34 above 3 GPa when following the same P–T evolution for metal–silicate equilibration in this study.

Our calculations followed the concepts of Rubie et al.60 except that impactor size and composition does not change during accretion. Upon each impact on the proto-Earth, an impactor core sinks in a descending plume, which expands with increasing depth as more silicate melt is turbulently entrained (see Fig. 2 in Deguen et al.61). The equilibrium efficiency between impactor metal and the proto-Earth’s silicate is controlled by Γ at each step, which is the ratio of the mass of equilibrated silicate over the mass of each impactor core. We performed 1000-step calculations of metal–silicate partitioning, with N (1–10) impactors for each step.

At ith step, Γi is obtained as follows. The volume fraction of metal (φmetal,i) in such metal + silicate composite plume when it reaches the bottom of the MO is given by Deguen et al.61,

$$\varphi _{{\mathrm{metal}},i} = \left( {\frac{{r_{{\mathrm{imp}}\,{\mathrm{core}}}}}{{r_{{\mathrm{plume}}}}}} \right)^3 = \left( {1 + \frac{{\alpha Z_i}}{{r_{{\mathrm{imp}}\,{\mathrm{core}}}}}} \right)^{ - 3}$$

in which α = 0.25, Zi is depth of the MO, and rimp core is the radius of impactor’s core. rimp core is formulated as:

$$r_{{\mathrm{imp}}\,{\mathrm{core}}} = \left[ {\frac{{m_{{\mathrm{imp}}} - \frac{4}{3}\pi \times r_{{\mathrm{imp}}}^3 \times \rho _{{\mathrm{imp}}\,{\mathrm{silicate}}}}}{{\frac{4}{3}\pi \times \left( {\rho _{{\mathrm{imp}}\,{\mathrm{core}}} - \rho _{{\mathrm{imp}}\,{\mathrm{silicate}}}} \right)}}} \right]^{1/3}$$

with impactor’s entire mass mimp (=1/1000/N × Earth’s mass), silicate and core densities ρimp silicate = (1.446/1000/N + 3) × 103 (kg m−3) and ρimp core = 2.5 × ρimp silicate6 and entire radius rimp of the impactor,

$$r_{{\mathrm{imp}}} = \left[ {\frac{{m_{{\mathrm{imp}}\,{\mathrm{silicate}}} + 0.4\,m_{{\mathrm{imp}}\,{\mathrm{core}}}}}{{\frac{4}{3}\pi \times \rho _{{\mathrm{imp}}\,{\mathrm{silicate}}}}}} \right]^{1/3}$$

Both the mass of impactor silicate and core, mimp silicate and mimp core, are obtained when ΦFe, ΦSi (the proportions of metallic Fe and Si with respect to all Fe and Si) and H2O concentration of the impactor are given. rimp is found, for example, to be 408 km when ΦFe = 0.99, ΦSi = 0.17, H2O=1.1 wt% and N = 1 (Supplementary Table 3). It could be argued that the average impactor size during Earth accretion was smaller (N > 1) considering the biggest asteroid Ceres is 473 km in radius.

Zi, the depth of the MO at step i, is given as rpEarth,i − rMOB,i. rpEarth,i is the radius of the entire embryo (proto-Earth), which is calculated using Eq. 7 with its silicate density ρpEarth silicate,i = (1.446 × i /1000 + 3) × 103 (kg m−3) and the mass of its silicate and core, mpEarth silicate,i and mpEarth core,i, that are calculated at each step. rMOB,i, the radius of the bottom of the MO, was obtained from the following equations with corresponding pressure PMOB,i = Pi (GPa) for metal–silicate equilibrium5,62,

$$P_{{\mathrm{MOB}},i} \times 10^9 = P_{{\mathrm{final}}} \times \left( {\frac{i}{{1000}}} \right)^{2/3} \times 10^9\\ = \frac{4}{3}\pi G\rho _{{\mathrm{pEarth}}\,{\mathrm{silicate}},\,i}\ r_{{\mathrm{MOB}},i}^3\left( {\rho _{{\mathrm{pEarth}}\,{\mathrm{core}},\,i} - \rho _{{\mathrm{pEarth}}\,{\mathrm{silicate}},\,i}} \right)\left( {\frac{1}{{r_{{\mathrm{MOB}},i}}} - \frac{1}{{r_{{\mathrm{pEarth}},i}}}} \right)\\ \ \ + \frac{2}{3}\pi G\rho _{{\mathrm{pEarth}}\,{\mathrm{silicate}},\,i}^2\left( {r_{{\mathrm{pEarth}},i}^2 - r_{{\mathrm{MOB}},i}^2}\right) $$

with gravitational constant G. For example, in an embryo with 1/10 Earth’s mass and a radius of ~3200 km, the depths of the core–mantle boundary and the bottom of the MO (Z100) are ~1500 and ~900 km, respectively, depending on ΦFe and ΦSi.

Finally Γ i is obtained as:

$$\Gamma _i = \frac{{m_{{\mathrm{equilibrated}}\,{\mathrm{silicate}}}^\prime }}{{m_{{\mathrm{imp}}\,{\mathrm{core}}}^\prime }} = \frac{{\frac{4}{3}\pi{}r_{{\mathrm{imp}}\,{\mathrm{core}}}^{\prime 3} \times \left( {\frac{1}{{\varphi _{{\mathrm{metal}},{i}}}} - 1} \right) \times \rho{}_{{\mathrm{pEarth}}\,{\mathrm{silicate}},{i}}}}{{m_{{\mathrm{imp}}\,{\mathrm{core}}}^\prime }}$$

with φmetal,i (Eq. 5) and the radius rimp core and mass mimp core of combined N impactors accreting in each 1/1000 step of metal–silicate partitioning. Eq. 9 indicates that Γi is larger (impactor core reacts with more silicate) when φmetal,i (namely, impactor size) is smaller. In addition, we considered that the impactor’s silicate was preferentially involved in the chemical reaction with the impactor metal in the MO (Supplementary Fig. 10).

We have calculated the partitioning of H, Ni, Co, O, and Si between the impactor metal and equilibrated silicate (whose mass is obtained by Γi) under PMOB,i = Pfinal × (i/1000)2/3 and three different T at each step (Supplementary Fig. 1):

  1. (1)

    TMOB1,i = (same as that for the continuous core formation model above).

  2. (2)

    TMOB2,i = 1940 × (PMOB,/29 + 1)1/1.9.

  3. (3)

    \(T_{{\mathrm{MOB3}},i}= \left\{\begin{array}{*{20}{l}}1874 + 55.43P_{{\mathrm{MOB}},i}- 1.74P_{{\mathrm{MOB}},i}^{2} + 0.0193P_{{\mathrm{MOB}},i}^{3 } (< 24 {\mathrm{GPa}}) \\ 1249 + 58.28P_{{\mathrm{MOB}},i}- 0.395P_{{\mathrm{MOB}},i}^{2} + 0.0011P_{{\mathrm{MOB}},i}^{3 } (\ge \,24 \,{\mathrm{GPa}})\end{array}\right.\)

For each of the three TMOB profiles, three different sets of metal–silicate partitioning data for Ni, Co, O, and Si2,3,6,57,63 were applied. Each impactor had a CI chondritic-like composition for refractory elements (see Table S1 in Rubie et al.6). The evolution of fO2 was calculated as \(\Delta {\mathrm{IW}} \approx - 2\log _{10}\frac{{x\prime _{{\mathrm{Fe}}}^{{\mathrm{metal}}}}}{{x_{{\mathrm{FeO}}}^{{\mathrm{silicate}}}}}\) (molar fraction x′ does not consider H in metal, see above) at each step, which is the consequences of the incorporation of H, Si, and O into core-forming metal and of Ni, Co and Fe into silicate. We did not consider the partitioning of S into silicate nor that of Al, Mg, and Ca into metal. We assumed that metal–silicate partitioning was not affected by the presence of H and H2O (see51,52 and Supplementary Fig. 8).

We have explored parameter sets of N, Pfinal, and impactor’s ΦFe, ΦSi, and H2O concentration, which explain the residual silicate abundances of ~700 ppm H2O, ~8.1 wt% FeO, ~2000 ppm Ni, and ~100 ppm Co59 (Fig. 4 and Supplementary Fig. 5). The mass fraction of the core, containing ~2 wt% S54 in addition to H, Ni, Co, O, and Si, was targeted to be 0.325. Supplementary Fig. 6 shows parameters search maps for reductive, moderate and oxidative impactor cases. With N = 3, TMOB1 and metal–silicate partitioning data reported by Siebert et al.2,57, homogeneous accretions of reductive but water-bearing impactors best explain the Earth’s composition (the evolution during accretion is given in Supplementary Data 1). We found a reasonable parameter set for each combination of three different P–T paths and three different sets of partitioning data2,3,6,57,63 as listed in Supplementary Table 3. These calculations show that hydrogen concentration ranges from 0.27 to 0.56 wt% in the Earth’s core (Supplementary Table 4). The evolutions of P, T, and fO2 conditions for metal–silicate equilibrium, core mass fraction, the FeO, Ni, Co, and H2O contents in the magma ocean, and the O, Si, and H abundances in the core are illustrated in Fig. 4 and Supplementary Fig. 5.

Pressure and temperature effects on hydrogen partitioning using previous low-pressure data along with the present results

We also estimated the effects of P and T on metal–silicate partitioning of hydrogen using earlier low-pressure multi-anvil experimental data12 along with the present results. The exchange coefficient KD is written as

$${\mathrm{log}}_{10}K_{\mathrm{D}} = 0.692\left( {986} \right) - 4590\left( {1690} \right)/T\left( {\mathrm{K}} \right) + 141\left( {43} \right) \,\times P\left( {{\mathrm{GPa}}} \right)/T\left( {\mathrm{K}} \right)$$

They are compared with those obtained only from our data in Supplementary Fig. 11.

With such parameters, we have additionally calculated the amount of hydrogen incorporated into the core on the basis of a multi-stage core formation model that is similar to model #S1 except for the KD value (Supplementary Fig. 12, and Supplementary Tables 3 and 4). The results show 0.34 wt% H in the core, consistent with those obtained by other simulations.

Data availability

The data supporting the main findings of this study are available in the paper and it’s Supplementary Information. Any additional data can be available from the corresponding authors upon reasonable request.


  1. Bouhifd, M. A. & Jephcoat, A. P. Convergence of Ni and Co metal–silicate partition coefficients in the deep magma-ocean and coupled silicon–oxygen solubility in iron melts at high pressures. Earth Planet. Sci. Lett. 307, 341–348 (2011).

    ADS  CAS  Article  Google Scholar 

  2. Siebert, J., Badro, J., Antonangeli, D. & Ryerson, F. J. Metal–silicate partitioning of Ni and Co in a deep magma ocean. Earth Planet. Sci. Lett. 321–322, 189–197 (2012).

    ADS  Article  CAS  Google Scholar 

  3. Fischer, R. A. et al. High pressure metal–silicate partitioning of Ni, Co, V, Cr, Si, and O. Geochim. Cosmochim. Acta 167, 177–194 (2015).

    ADS  CAS  Article  Google Scholar 

  4. Wade, J. & Wood, B. J. Core formation and the oxidation state of the Earth. Earth Planet. Sci. Lett. 236, 78–95 (2005).

    ADS  CAS  Article  Google Scholar 

  5. Badro, J., Brodholt, J. P., Piet, H., Siebert, J. & Ryerson, F. J. Core formation and core composition from coupled geochemical and geophysical constraints. Proc. Natl Acad. Sci. USA 112, 12310–12314 (2015).

    ADS  CAS  PubMed  Article  PubMed Central  Google Scholar 

  6. Rubie, D. C. et al. Accretion and differentiation of the terrestrial planets with implications for the compositions of early-formed Solar System bodies and accretion of water. Icarus 248, 89–108 (2015).

    ADS  CAS  Article  Google Scholar 

  7. Li, J. & Fei, Y. Experimental constraints on core composition. In Treatise on Geochemistry 2nd edn, Vol. 3 (eds. Holland, H. D. & Turekian, K. K.) 527–557 (Elsevier, 2014).

  8. Okuchi, T. Hydrogen partitioning into molten iron at high pressure: implications for Earth’s core. Science 278, 1781–1784 (1997).

    ADS  CAS  PubMed  Article  PubMed Central  Google Scholar 

  9. Shibazaki, Y., Ohtani, E., Terasaki, H., Suzuki, A. & Funakoshi, K. Hydrogen partitioning between iron and ringwoodite: implications for water transport into the Martian core. Earth Planet. Sci. Lett. 287, 463–470 (2009).

    ADS  CAS  Article  Google Scholar 

  10. Iizuka-Oku, R. et al. Hydrogenation of iron in the early stage of Earth’s evolution. Nat. Commun. 8, 14096 (2017).

    ADS  CAS  PubMed  PubMed Central  Article  Google Scholar 

  11. Clesi, V. et al. Low hydrogen contents in the cores of terrestrial planets. Sci. Adv. 4, e1701876 (2018).

    ADS  PubMed  PubMed Central  Article  CAS  Google Scholar 

  12. Malavergne, V. et al. Experimental constraints on the fate of H and C during planetary core-mantle differentiation. Implications for the Earth. Icarus 321, 473–485 (2019).

    ADS  CAS  Article  Google Scholar 

  13. Zhang, Y. & Yin, Q.-Z. Carbon and other light element contents in the Earth’s core based on first-principles molecular dynamics. Proc. Natl Acad. Sci. USA 109, 19579–19583 (2012).

    ADS  CAS  PubMed  Article  PubMed Central  Google Scholar 

  14. Li, Y., Vočadlo, L., Sun, T. & Brodholt, J. P. The Earth’s core as a reservoir of water. Nat. Geosci. 13, 453–458 (2020).

    ADS  CAS  Article  Google Scholar 

  15. Yuan, L. & Steinle-Neumann, G. Strong sequestration of hydrogen into the Earth’s core during planetary differentiation. Geophys. Res. Lett. 47, e2020GL088303 (2020).

    ADS  CAS  Google Scholar 

  16. Fukai, Y. & Suzuki, T. Iron–water reaction under high pressure and its implication in the evolution of the Earth. J. Geophys. Res. 91, 9222 (1986).

    ADS  CAS  Article  Google Scholar 

  17. Hirose, K. et al. Hydrogen limits carbon in liquid iron. Geophys. Res. Lett. 46, 5190–5197 (2019).

    ADS  CAS  Article  Google Scholar 

  18. Hirschmann, M. M. Constraints on the early delivery and fractionation of Earth’s major volatiles from C/H, C/N, and C/S ratios. Am. Mineral. 101, 540–553 (2016).

    ADS  Article  Google Scholar 

  19. Lécuyer, C., Gillet, P. & Robert, F. The hydrogen isotope composition of seawater and the global water cycle. Chem. Geol. 145, 249–261 (1998).

    ADS  Article  Google Scholar 

  20. Pope, E. C., Bird, D. K. & Rosing, M. T. Isotope composition and volume of Earth’s early oceans. Proc. Natl Acad. Sci. USA 109, 4371–4376 (2012).

    ADS  CAS  PubMed  Article  PubMed Central  Google Scholar 

  21. Zahnle, K. J., Gacesa, M. & Catling, D. C. Strange messenger: a new history of hydrogen on Earth, as told by xenon. Geochim. Cosmochim. Acta 244, 56–85 (2019).

    ADS  CAS  Article  Google Scholar 

  22. Wang, Z. & Becker, H. Ratios of S, Se and Te in the silicate Earth require a volatile-rich late veneer. Nature 499, 328–331 (2013).

    ADS  CAS  PubMed  Article  PubMed Central  Google Scholar 

  23. Umemoto, K. & Hirose, K. Liquid iron‐hydrogen alloys at outer core conditions by first‐principles calculations. Geophys. Res. Lett. 42, 7513–7520 (2015).

    ADS  CAS  Article  Google Scholar 

  24. Umemoto, K. & Hirose, K. Chemical compositions of the outer core examined by first principles calculations. Earth Planet. Sci. Lett. 531, 116009 (2020).

    CAS  Article  Google Scholar 

  25. Wu, J. et al. Origin of Earth’s water: chondritic inheritance plus nebular ingassing and storage of hydrogen in the core. J. Geophys. Res. Planets 123, 2691–2712 (2018).

    ADS  CAS  Article  Google Scholar 

  26. Hallis, L. J. et al. Evidence for primordial water in Earth’s deep mantle. Science 350, 336–339 (2015).

    Article  CAS  Google Scholar 

  27. Mundl-Petermeier, A. et al. Anomalous 182W in high 3He/4He ocean island basalts: fingerprints of Earth’s core? Geochim. Cosmochim. Acta 271, 194–211 (2020).

    ADS  CAS  Article  Google Scholar 

  28. Walsh, K. J., Morbidelli, A., Raymond, S. N., O’Brien, D. P. & Mandell, A. M. A low mass for Mars from Jupiter’s early gas-driven migration. Nature 475, 206–209 (2011).

    ADS  CAS  PubMed  Article  PubMed Central  Google Scholar 

  29. Sato, T., Okuzumi, S. & Ida, S. On the water delivery to terrestrial embryos by ice pebble accretion. Astron. Astrophys. 589, A15 (2016).

    ADS  Article  CAS  Google Scholar 

  30. Raymond, S. N., Quinn, T. & Lunine, J. I. High-resolution simulations of the final assembly of Earth-like planets. 2. Water delivery and planetary habitability. Astrobiology 7, 66–84 (2007).

    ADS  CAS  PubMed  Article  PubMed Central  Google Scholar 

  31. Hirose, K., Fei, Y., Ma, Y. & Mao, H. The fate of subducted basaltic crust in the Earth’s lower mantle. Nature 397, 53–56 (1999).

    ADS  CAS  Article  Google Scholar 

  32. Tateno, S. et al. Melting phase relations and element partitioning in MORB to lowermost mantle conditions. J. Geophys. Res. Solid Earth 123, 5515–5531 (2018).

    ADS  Article  Google Scholar 

  33. Helffrich, G. Outer core compositional layering and constraints on core liquid transport properties. Earth Planet. Sci. Lett. 391, 256–262 (2014).

    ADS  CAS  Article  Google Scholar 

  34. de Koker, N. P., Stixrude, L. & Karki, B. B. Thermodynamics, structure, dynamics, and freezing of Mg2SiO4 liquid at high pressure. Geochim. Cosmochim. Acta 72, 1427–1441 (2008).

    ADS  Article  CAS  Google Scholar 

  35. Mori, Y. et al. Melting experiments on Fe–Fe3S system to 254 GPa. Earth Planet. Sci. Lett. 464, 135–141 (2017).

    ADS  CAS  Article  Google Scholar 

  36. Akahama, Y. & Kawamura, H. High-pressure Raman spectroscopy of diamond anvils to 250 GPa: method for pressure determination in the multimegabar pressure range. J. Appl. Phys. 96, 3748–3751 (2004).

    ADS  CAS  Article  Google Scholar 

  37. Andrault, D. et al. Solidus and liquidus profiles of chondritic mantle: implication for melting of the Earth across its history. Earth Planet. Sci. Lett. 304, 251–259 (2011).

    ADS  CAS  Article  Google Scholar 

  38. Fukai, Y. Some properties of the Fe-H system at high pressures and temperatures, and their implications for the Earth’s core. In High-Pressure Research: Applications to Earth and Planetary Sciences Vol. 67 (eds. Syono, Y. & Manghnani, M. H.) 373–385 (TERRAPUB, 1992).

  39. Caracas, R. The influence of hydrogen on the seismic properties of solid iron. Geophys. Res. Lett. 42, 3780–3785 (2015).

    ADS  CAS  Article  Google Scholar 

  40. Machida, A. et al. Site occupancy of interstitial deuterium atoms in face-centred cubic iron. Nat. Commun. 5, 5063 (2014).

    ADS  CAS  PubMed  PubMed Central  Article  Google Scholar 

  41. Ikuta, D. et al. Interstitial hydrogen atoms in face-centered cubic iron in the Earth’s core. Sci. Rep. 9, 7108 (2019).

    ADS  PubMed  PubMed Central  Article  CAS  Google Scholar 

  42. Dewaele, A. et al. Quasihydrostatic equation of state of iron above 2 Mbar. Phys. Rev. Lett. 97, 215504 (2006).

    ADS  PubMed  Article  CAS  PubMed Central  Google Scholar 

  43. Tsujino, N. et al. Equation of state of γ-Fe: reference density for planetary cores. Earth Planet. Sci. Lett. 375, 244–253 (2013).

    ADS  CAS  Article  Google Scholar 

  44. Thompson, E. C., Campbell, A. J. & Tsuchiya, J. Elasticity of ε-FeOOH: seismic implications for Earth’s lower mantle. J. Geophys. Res. Solid Earth 122, 5038–5047 (2017).

    ADS  CAS  Article  Google Scholar 

  45. Yurimoto, H., Nagashima, K. & Kunihiro, T. High precision isotope micro-imaging of materials. Appl. Surf. Sci. 203–204, 793–797 (2003).

    ADS  Article  Google Scholar 

  46. Greenwood, J. P. et al. Hydrogen isotope ratios in lunar rocks indicate delivery of cometary water to the Moon. Nat. Geosci. 4, 79–82 (2011).

    ADS  CAS  Article  Google Scholar 

  47. Sakamoto, N. et al. Remnants of the early solar system water enriched in heavy oxygen isotopes. Science 317, 231–233 (2007).

    ADS  CAS  PubMed  Article  PubMed Central  Google Scholar 

  48. Yamamoto, K., Sakamoto, N. & Yurimoto, H. Analysis of the noise properties of a solid-state SCAPS ion imager and development of software noise reduction. Surf. Interface Anal. 42, 1603–1605 (2010).

    CAS  Article  Google Scholar 

  49. Yoshimura, S. Diffusive fractionation of H2O and CO2 during magma degassing. Chem. Geol. 411, 172–181 (2015).

    ADS  CAS  Article  Google Scholar 

  50. Fukai, Y. The Metal-Hydrogen System. Vol. 21 (Springer-Verlag, 2005).

  51. Righter, K. & Drake, M. J. Effect of water on metal–silicate partitioning of siderophile elements: a high pressure and temperature terrestrial magma ocean and core formation. Earth Planet. Sci. Lett. 171, 383–399 (1999).

    ADS  CAS  Article  Google Scholar 

  52. Clesi, V. et al. Effect of H2O on metal–silicate partitioning of Ni, Co, V, Cr, Mn and Fe: implications for the oxidation state of the Earth and Mars. Geochim. Cosmochim. Acta 192, 97–121 (2016).

    ADS  CAS  Article  Google Scholar 

  53. Takahashi, E. Melting of a dry peridotite KLB-1 up to 14 GPa: implications on the origin of peridotitic upper mantle. J. Geophys. Res. 91, 9367–9382 (1986).

    ADS  CAS  Article  Google Scholar 

  54. McDonough, W. F. Compositional model for the Earth’s core. In Treatise on Geochemistry 2nd edn, Vol. 3 (eds. Holland, H. D. & Turekian, K. K.) 559–577 (Elsevier, 2014).

  55. Badro, J., Cote, A. S. & Brodholt, J. P. A seismologically consistent compositional model of Earth’s core. Proc. Natl Acad. Sci. USA 111, 7542–7545 (2014).

    ADS  CAS  PubMed  Article  PubMed Central  Google Scholar 

  56. Hirose, K. et al. Crystallization of silicon dioxide and compositional evolution of the Earth’s core. Nature 543, 99–102 (2017).

    ADS  CAS  PubMed  Article  PubMed Central  Google Scholar 

  57. Siebert, J., Badro, J., Antonangeli, D. & Ryerson, F. J. Terrestrial accretion under oxidizing conditions. Science 339, 1194–1197 (2013).

    ADS  CAS  PubMed  Article  PubMed Central  Google Scholar 

  58. Dauphas, N. The isotopic nature of the Earth’s accreting material through time. Nature 541, 521–524 (2017).

    ADS  CAS  PubMed  Article  PubMed Central  Google Scholar 

  59. McDonough, W. F. & Sun, S. The composition of the Earth. Chem. Geol. 120, 223–253 (1995).

    ADS  CAS  Article  Google Scholar 

  60. Rubie, D. C. et al. Heterogeneous accretion, composition and core-mantle differentiation of the Earth. Earth Planet. Sci. Lett. 301, 31–42 (2011).

    ADS  CAS  Article  Google Scholar 

  61. Deguen, R., Olson, P. & Cardin, P. Experiments on turbulent metal–silicate mixing in a magma ocean. Earth Planet. Sci. Lett. 310, 303–313 (2011).

    ADS  CAS  Article  Google Scholar 

  62. Turcotte, D. & Schubert, G. Geodynamics 3rd edn (Cambridge University Press, 2014).

  63. Mann, U., Frost, D. J. & Rubie, D. C. Evidence for high-pressure core-mantle differentiation from the metal–silicate partitioning of lithophile and weakly-siderophile elements. Geochim. Cosmochim. Acta 73, 7360–7386 (2009).

    ADS  CAS  Article  Google Scholar 

  64. Peslier, A. H., Schönbächler, M., Busemann, H. & Karato, S. I. Water in the Earth’s interior: distribution and origin. Space Sci. Rev. 212, 1–68 (2017).

    Article  Google Scholar 

  65. Palme, H. & O’Neill, H. S. C. Cosmochemical estimates of mantle composition. In Treatise on Geochemistry 2nd edn, Vol. 3 (eds. Holland, H. D. & Turekian, K. K.) 1–39 (Elsevier, 2014).

Download references


We thank N. Hirao and S. Kawaguchi for their assistance in experiments at BL10XU, SPring-8 (proposal no. 2018A0072 and 2018B0072). S. Yoshimura is acknowledged for preparing standards for SIMS analyses. K. Yonemitsu supports FIB analyses. We also thank M. Takei and M. Kusuzaki for sample holder development. Comments from M. Bouhifd and two anonymous referees were helpful to improve the manuscript. This work was supported by JSPS Kakenhi to K.H. and H.Y. and fellowship to S.T., and by the “Imaging Platform” program by MEXT.

Author information




S.T. designed and led the project together with K.H. and H.Y. High-pressure experiments and SIMS analyses were performed by Y.O. and N.S., respectively. S.T., K.H., and S.Y. performed computational simulations. S.T, K.H., and J.H. wrote the manuscript, and all authors commented on it.

Corresponding authors

Correspondence to Shoh Tagawa or Kei Hirose.

Ethics declarations

Competing interests

The authors declare no competing interests.

Additional information

Peer review information Nature Communications thanks Jie Li and the other, anonymous reviewers for their contribution to the peer review of this work.

Publisher’s note Springer Nature remains neutral with regard to jurisdictional claims in published maps and institutional affiliations.

Supplementary information

Rights and permissions

Open Access This article is licensed under a Creative Commons Attribution 4.0 International License, which permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons license, and indicate if changes were made. The images or other third party material in this article are included in the article’s Creative Commons license, unless indicated otherwise in a credit line to the material. If material is not included in the article’s Creative Commons license and your intended use is not permitted by statutory regulation or exceeds the permitted use, you will need to obtain permission directly from the copyright holder. To view a copy of this license, visit

Reprints and Permissions

About this article

Verify currency and authenticity via CrossMark

Cite this article

Tagawa, S., Sakamoto, N., Hirose, K. et al. Experimental evidence for hydrogen incorporation into Earth’s core. Nat Commun 12, 2588 (2021).

Download citation

  • Received:

  • Accepted:

  • Published:

  • DOI:

Further reading


By submitting a comment you agree to abide by our Terms and Community Guidelines. If you find something abusive or that does not comply with our terms or guidelines please flag it as inappropriate.


Quick links

Nature Briefing

Sign up for the Nature Briefing newsletter — what matters in science, free to your inbox daily.

Get the most important science stories of the day, free in your inbox. Sign up for Nature Briefing