Cores Of Bodies Research Articles

The direction of core solidification in asteroids: Implications for dynamo generation

Paleomagnetic studies of meteorites over the past two decades have revealed that the cores of multiple meteorite parent bodies, including those of certain chondritic groups, generated dynamo fields as they crystallised. However, uncertainties in the direction and mode of core solidification in asteroid-sized bodies have meant using the timings and durations of these fields to constrain parent body properties, such as size, is challenging. Here, we use updated equations of state and liquidus relationships for Fe-FeS liquids at low pressures to calculate the locations at which solids form in these cores. We perform these calculations for core-mantle boundary (CMB) pressures from 0–2 GPa, and Fe-FeS liquid concentrations on the iron-rich side of the eutectic, as well as two values of iron thermal expansivity that cover the measured uncertainties in this parameter, and adiabatic and conductive cooling of these cores. We predict inward core crystallisation from the CMB in asteroids due to their low < 0.5 GPa pressures regardless of the uncertainties in other key core parameters. However, due to low internal pressures in these cores, remelting of any iron snow, as proposed to generate Ganymede’s present-day field, may be unlikely as the cores are approximately isothermal. Therefore a different mode of inward core solidification is possibly required to explain compositionally-driven dynamo action in asteroids. Additionally, we identify possible regimes at higher > 0.6 − 2 GPa pressures in which crystallisation can occur concurrently at the CMB and the centre.

Sound Velocities of Fe‐Si Alloys at Conditions of the Cores of Moon and Mercury

AbstractThe species and contents of the light elements within the metallic cores play a crucial role in understanding the structure, thermal state, geodynamo, and evolution of the terrestrial planets and satellites. While silicon (Si) has been considered as a primary candidate light element in the cores of small terrestrial bodies, the sound velocities of face‐centered cubic (fcc) Fe‐Si are rarely investigated. Here we measured the compressional (VP) and shear (VS) wave velocities of Fe alloyed with 3 wt.% and 6 wt.% Si up to 6.3 GPa and 1,273 K using pulse‐echo overlap technique coupled with energy‐dispersive X‐ray diffraction. The incorporation of Si could increase the VP of body‐centered cubic (bcc) Fe by 0.074(15) km/s and decrease the VS by 0.024(9) km/s with each weight percent Si at 300 K. However, 3 wt.% Si has minimal effect on the VP of fcc‐Fe if not negligible. The incorporation of 6 wt.% Si stabilizes the Fe in mixture bcc and fcc phases at high temperature and increases the VP by 0.59 km/s compared with that of fcc‐Fe. Based on the Apollo seismic observation and VP of Fe and Fe‐Si alloys, Si is unlikely to be the sole light element in the lunar core. The solid core of the Mercury would be in the fcc phase if the Si content is less than 3 wt.% and the VP profiles is 5.65–6.34 km/s. While 6 wt.% Si would stabilize the Mercury's core in mixed bcc and fcc phases, the VP profiles would be 6.17–6.85 km/s.

Nitrogen inventory of iron meteorite parent bodies constrained by nitrogen partitioning between Fe-rich solid and liquid alloys

Delivery of nitrogen (N), one of the most important elements for life, to Earth thought to have occurred via both undifferentiated and differentiated bodies, lasting at least 50–100 Ma from the birth of the Solar System. Therefore, to understand how Earth got its N, it is imperative to know the N budget of the earliest formed bodies in our Solar System. The best astromaterials available for providing constraints on N budget of the earliest formed planetesimals are the iron meteorites. However, iron meteorites are crystallized products of a liquid alloy and do not represent the N budget of the bulk cores of various iron meteorite parent bodies (IMPBs). Therefore, to determine how N partitioned between solid alloy (sa) and liquid alloy (la) (DNsa/la) during crystallization of molten metal alloy core, we present a series of equilibrium partitioning experiments at 1–2 GPa and 1150–1550 ℃ for various initial starting compositions having different sulfur (S), nickel (Ni), iron (Fe) and fixed nitrogen (N) concentrations. We observe that N changes from mildly incompatible to mildly compatible with increasing S concentration in the liquid alloy. Furthermore, we observed that N concentration in solid alloy decreases with increasing temperature, while pressure and Ni content showed almost no effect on the partitioning behavior of N. We used a regression model based on the results of our study and a previous study to establish a parameterization for DNsa/la. Using our parameterized DNsa/la, we determine potential siderophile element proxies of N in metallic systems and model the initial N budget of various IMPBs groups pertaining to the inner (Non-Carbonaceous (NC) reservoir) and outer Solar System (Carbonaceous (CC) reservoir). Between two possible end-member styles of IMPB differentiation (IMO – Internal Magma Ocean; EMO – External Magma Ocean), EMOs result in a higher initial N budget with a major fraction getting lost via atmospheric loss. Importantly, our calculations suggest a gradation in the N budget of CC and NC IMPBs with CC IMPBs hosting lesser N than NC IMPBs. Therefore, the early Solar protoplanetary disk likely showed a gradation in N both in its elemental and isotopic composition.

A two-phase pure slurry model for planetary cores: one-dimensional solutions and implications for Earth's F-layer

We develop and analyse a continuum model of two-phase slurry dynamics for planetary cores. Mixed solid–liquid slurry regions may be ubiquitous in the upper cores of small terrestrial bodies and have also been invoked to explain anomalous seismic structure in the F-layer at the base of Earth's liquid iron core. These layers are expected to influence the dynamics and evolution of planetary cores, including their capacity to generate global magnetic fields; however, to date, models of two-phase regions in planetary cores have largely ignored the complex fluid dynamics that arises from interactions between phases. As an initial application of our model, and to focus on fundamental fluid dynamical processes, we consider a non-rotating and non-magnetic slurry comprised of a single chemical component with a temperature that is tied to the liquidus. We study one-dimensional solutions in a configuration set up to mimic Earth's F-layer, varying gravitational strength$R$, the solid/liquid viscosity ratio$\lambda _{\mu }$and the interaction parameter$K$, which measures friction between the phases. We develop scalings describing behaviour in the limit$R \gg 1$and$\lambda _{\mu } \gg 1$, which are in excellent agreement with our numerical results. Application to Earth's core, where$R \sim 10^{28}$and$\lambda _{\mu } \sim 10^{22}$, suggests that a pure iron slurry F-layer would contain a mean solid fraction of at most 5 %.

Electrical resistivity of liquid Fe-8wt%S-4.5wt%Si at high pressures with implications for heat flux through the cores of Io and sub-earth exoplanets

Potentially resulting in magnetic dynamo action, the heat flow through the outer cores of small terrestrial planetary bodies depends on the thermal conductivity of liquid Fe alloys at high pressures. The electrical resistivity of liquid Fe-8wt%S-4.5wt%Si was measured at 2–5 GPa and 295–1800 K in a 1000-ton cubic anvil press with a sample volume of a few cubic millimeters. Resistivity values of 220–270 μΩ·cm were measured, and a range of thermal conductivity values of 15–19 W/m/K were calculated using the Wiedemann-Franz law. The adiabatic heat flux at the top of a terrestrial exoplanet's Fe-8wt%S-4.5wt%Si core as a function of radius is calculated. The core of Io, if liquid, could have a convective heat flow density of a few μW/m2 without generating a magnetic dynamo powered by thermal convection.

High P-T experimental perspective on Cr isotopic fractionation during planetary core formation

Core formation may modify the stable isotopic signatures for both the mantles and cores of differentiated planetary bodies. We performed high P-T experiments with a piston-cylinder apparatus at 1 GPa and 1873-2073 K to determine the Cr isotopic fractionation factor during metal-silicate segregation. Experimental results consistently indicate that the metal phase is isotopically heavier than the coexisting silicate phase, with Δ53Crmetal-silicate up to 0.3‰ at the investigated experimental conditions. Oxygen fugacity, silicate composition, and S content in the metal phase do not have significant effects on the Cr isotopic fractionation factor. By contrast, increasing Ni content in the metal increases the Δ53Crmetal-silicate value, implying that the Ni content of the core could influence planetary isotopic signatures. We conclude that heavier Cr isotopes enter the core preferentially during planetary core formation. The δ53Cr value of the terrestrial mantle could be lowered by up to ∼0.02‰ by core formation, despite that this is within current analytical uncertainty of chondritic Cr isotopic composition. For smaller bodies such as the Moon, Mars, and Vesta, the lower core formation temperatures could potentially generate a resolvable core-mantle Cr isotopic fractionation. However, the Moon's small core size would limit the change in the Cr isotopic composition of the lunar mantle compared to chondritic. For Vesta and Mars, core formation could lower the δ53Cr values of their mantles by ∼0.01-0.02‰, which is trivial relative to the analytical uncertainty. On the other hand, core formation could increase the δ53Cr values of the cores of the parent bodies of iron meteorites by up to ∼0.2‰ at 1873 K. Therefore, the significantly heavy Cr isotopic composition (up to 2.85‰) of iron meteorites cannot be explained by equilibrium fractionation between the core and the mantle of the parent bodies of iron meteorites.

Terrigenous organic matter and formation of siderite in the Bathonian Ore-Bearing Clay Formation at Gnaszyn, Poland – a petrochemical study

The Bathonian Ore-Bearing Clay Formation, outcropping in the Gnaszyn open-pit mine at Częstochowa (Poland), includes several horizons of abundant iron carbonate concretions . The cores of the concretionary bodies commonly contain organic matter (OM), dominated by fragments of wood. These organic particles usually display well-preserved primary structures and occur rarely as more deformed and/or completely degraded fragments. Their original structures are frequently replaced by or filled with secondary mineralization, mostly represented by pyrite. The maceral composition of the OM of the wood fragments is dominated by huminite with subordinate inertinite and resinite. Vitrinite reflectance analyses revealed values lower than 0.45%. The total organic carbon content (TOC) displayed variable results between 2% and 18%. Rock-Eval analyses revealed low amounts of hydrogen (&lt; 45 mg HC/g TOC) and relatively high amounts of oxygen (up to 136 mg CO 2 /g TOC). Analysed samples contained small quantities of free hydrocarbons (S1 peak &lt; 0.26 mg HC/g rock) as well as hydrocarbons, generated during pyrolysis (S2 peak &lt; 7.05 mg HC/g rock). These features are characteristic for immature type IV kerogen of terrigenous origin. However, the maceral composition and frequent occurrence of siderite affecting the Rock-Eval parameters may indicate that the original kerogen belonged to type III. According to previous authors, the OM of terrigenous origin was delivered to well-oxygenated water of the palaeo-basin in the Częstochowa area. The present data indicate that intensive biodegradation of this OM at shallow burial depleted the oxygen supply within the sediment, driving the pore water into dys- or anoxic conditions. The activity of microorganisms in reducing iron and/or sulphates became the dominant biodegradation reaction, introducing Fe 2+ and HCO 3 - ions into the system. Negative δ 13 C values in the cortex of the concretions analysed indicate that the bicarbonate consumed in siderite precipitation was supplied by this microbial activity. The reducing microenvironments developed in the sediment and wood fragments acted as nucleation sites for siderite precipitation.

Review of Electrical Resistivity Measurements and Calculations of Fe and Fe-Alloys Relating to Planetary Cores

There is a considerable amount of literature on the electrical resistivity of iron at Earth’s core conditions, while only few studies have considered iron and iron-alloys at other planetary core conditions. Much of the total work has been carried out in the past decade and a review to collect data is timely. High pressures and temperatures can be achieved with direct measurements using a diamond-anvil cell, a multi-anvil press or shock compression methods. The results of direct measurements can be used in combination with first-principle calculations to extrapolate from laboratory temperature and pressure to the relevant planetary conditions. This review points out some discrepancies in the electrical resistivity values between theoretical and experimental studies, while highlighting the negligible differences arising from the selection of pressure and temperature values at planetary core conditions. Also, conversions of the reported electrical resistivity values to thermal conductivity via the Wiedemann-Franz law do not seem to vary significantly even when the Sommerfeld value of the Lorenz number is used in the conversion. A comparison of the rich literature of electrical resistivity values of pure Fe at Earth’s core-mantle boundary and inner-core boundary conditions with alloys of Fe and light elements (Si, S, O) does not reveal dramatic differences. The scarce literature on the electrical resistivity at the lunar core suggests the effect of P on a wt% basis is negligible when compared to that of Si and S. On the contrary, studies at Mercury’s core conditions suggest two distinct groups of electrical resistivity values but only a few studies apply to the inner-core boundary. The electrical resistivity values at the Martian core-mantle boundary conditions suggest a negligible contribution of Si, S and O. In contrast, Fe-S compositions at Ganymede’s core-mantle boundary conditions result in large deviations in electrical resistivity values compared to pure Fe. Contour maps of the reported values illustrate ρ(P, T) for pure Fe and its alloys with Ni, O and Si/S and allow for estimates of electrical resistivity at the core-mantle boundary and inner-core boundary conditions for the cores of terrestrial-like planetary bodies.

Technique, cell assembly, and measurement of T-dependent electrical resistivity of liquid Fe devoid of contamination at P, T conditions.

Since the cores of rocky planetary bodies are mainly Fe in composition, the understanding of the electrical resistivity and thermal conductivity of solid and molten Fe at pressure and temperature conditions is vital in placing a constraint on the quantity of heat flux from the cores of these planets. We develop an experimental technique and cell design to measure the temperature-dependent electrical resistivity of solid and molten Fe and other transition metals under high pressure. This addresses the problem of metal sample contamination encountered in designs that used W/Re, W, and Mo in direct contact with the sample. At first, we attempted to improve these pre-existing designs by testing the suitability of Hf and Zr metals to serve as a mechanical barrier between the electrodes and the sample. Unfortunately, our result shows that solid Hf and Zr dissolve in molten Fe and are not suitable for this purpose. Next, we adopt the same sample material, Fe, for electrodes and leads while the thermocouple leads are taken through the gasket and protected against frequent mechanical breakage using the shielding technique. The recovered Fe samples compressed at various pressure conditions and heated up to 200 K above the melting temperature show no trace of contamination. As anticipated, the resistivity increases and decreases with increasing temperature and pressure, respectively. Thus, to closely measure the electrical resistivity of molten Fe and other similar metals at extreme conditions, it is necessary to ensure liquid containment, eliminate biased voltage through the current reversal technique, and ensure the use of the same material for the electrode and sample while monitoring the sample temperature using a thermocouple placed close to but not in contact with the sample. Our developed technique provides the highly demanding technique for investigating the temperature-dependent electrical resistivity of Fe and other similar metals devoid of contamination at extreme conditions. This progress will accelerate studies which will provide a detailed understanding of the electrical and heat transport properties of Fe as it applies to the core of rocky planetary bodies.

Liquid Iron Equation of State to the Terapascal Regime From Ab Initio Simulations

AbstractWe present a thermodynamic model for liquid iron, based on ab initio molecular dynamics simulations, which is applicable to 2 TPa and beyond 10000 K, conditions that are relevant in the cores of super‐Earths. We combine ab initio results for V‐T‐P‐E with a correction scheme to match experimental properties at ambient pressure, where ab initio results show poor agreement. We explore the performance of our thermodynamic potential and various previously published models for liquid iron over a wide range of conditions: (i) at ambient pressure as a function of temperature, (ii) along the melting curve of Fe to 40 GPa, relevant for the cores of smaller terrestrial bodies in our solar system, (iii) along isentropes in the Earth's outer core, and (iv) for the core of super‐Earth Kepler‐36b. The correction term significantly improves the agreement of computed properties with experiments and other thermodynamic models that are based on an assessment of the phase diagram at ambient and moderate pressure, showing how ab initio molecular dynamics simulations can be used at par with other thermodynamic techniques. For the Earth's core, densities from the various models are similar, but higher‐order derivatives (acoustic velocities and Grüneisen parameter) show significant differences. Evaluated along a core‐temperature profile in Kepler‐36b, differences in density from various models are negligible, for core mass they do not exceed 2%, showing robust extrapolation of all equation of state models.

Electrical resistivity of liquid Fe to 12\u2009GPa: Implications for heat flow in cores of terrestrial bodies

Electrical and thermal transport properties of liquid Fe under high pressure have important implications for the dynamics and thermal evolution of planetary cores and the geodynamo. However, electrical resistivity (ρ) and thermal conductivity (k) of liquid Fe at high pressure still remain contentious properties. To date, only two experimental investigations of ρ of liquid Fe in the pressure region below 7 GPa are reported in literature. Here we report the results of measurements of ρ for solid and liquid Fe (inversely proportional to k through the Wiedemann-Franz law) at pressures from 3 to 12 GPa, using a large multi-anvil press. We show that ρ of liquid Fe decreases as a function of pressure up to the δ-γ-liquid triple point at ~5.2 GPa, and subsequently remains invariant from 6 to 12 GPa, which is consistent with an earlier study on liquid Ni. Our results demonstrate an important effect of solid phase on the structure and properties of liquid Fe. Our values of ρ for solid and liquid Fe are used to calculate k in Mercury’s solid inner core and along the adiabat in the liquid outer cores of Moon, Ganymede, Mercury and Mars. Our robust values of thermal conductivity place the focus on uncertainties in thermal expansion as the cause of variation in values of core conducted heat. Except for Mercury, our adiabatic heat flux values in these terrestrial cores validate the use of similar values used in several previous studies. Our high values of core adiabatic heat flux in Mercury would provide a stabilizing effect on, and lead to an increase in thickness of, the thermally stratified layer at the top of the core.

Pressure Dependence of the Liquidus and Solidus Temperatures in the Fe‐P Binary System Determined by In Situ Ultrasonics: Implications to the Solidification of Fe‐P Liquids in Planetary Cores

AbstractWe have developed a new technique for determining the liquidus and eutectic (or solidus) temperatures of Fe‐light element alloys at high pressures in a multianvil apparatus, by studying ultrasonic wave propagation through the sample. While the onset of melting is manifested by the loss of both compressional (P‐) and shear (S‐) wave signals due to the scattering of sound waves by partial melts, the completion of melting is confirmed by the reappearance of the P wave signal when the scattering due to residual crystals disappears. By applying this technique to the Fe‐P binary system with three different phosphorus contents, we were able to constrain the Fe‐rich portion of the phase diagram up to 7 GPa and 1,733 K. Our results show that for phosphorus‐poor compositions, ranging from Fe‐5wt%P to the eutectic composition, the liquidus temperature exhibits a weak negative pressure dependence (dT/dP = −10.4 K GPa−1 for Fe‐5wt%P). While for the phosphorus‐richer compositions, including Fe‐10wt%P and Fe3P, the liquidus temperature increases significantly with pressure (dT/dP = 71.3 and 62.5 K GPa−1, respectively). This indicates a shift of the eutectic composition to lower phosphorus contents with increasing pressure. Consequently, molten metallic cores of planetary bodies with phosphorus contents ranging from Fe‐5wt%P to the eutectic composition would start crystallization from the top of the core and proceed downward. Whereas cores with phosphorus‐richer compositions (Fe‐10wt%P to Fe3P) would undergo a bottom‐up crystallization, resulting in a growing solid inner core.

Uranium isotope ratios of Muonionalusta troilite and complications for the absolute age of the IVA iron meteorite core

The crystallization ages of planetary crustal material (given by basaltic meteorites) and planetary cores (given by iron meteorites) provide fiducial marks for the progress of planetary formation, and thus, the absolute ages of these objects fundamentally direct our knowledge and understanding of planet formation and evolution. The lone precise absolute age of planetary core material was previously obtained on troilite inclusions from the IVA iron meteorite Muonionalusta. This previously reported Pb–Pb age of 4565.3 ± 0.1 Ma—assuming a 238U/235U =137.88—only post-dated the start of the Solar System by approximately 2–3 million years, and mandated fast cooling of planetary core material. Since an accurate Pb–Pb age requires a known 238U/235U of the sample, we have measured both 238U/235U and Pb isotopic compositions of troilite inclusions from Muonionalusta. The measured 238U/235U of the samples range from ∼137.84 to as low as ∼137.22, however based on Pb and U systematics, terrestrial contamination appears pervasive and has affected samples to various extents for Pb and U. The cause of the relative 235U excess in one sample does not appear to be from terrestrial contamination or the decay of short-lived 247Cm, but is more likely from fractionation of U isotopes during metal–silicate separation during core formation, exacerbated by the extreme U depletion in the planetary core. Due to limited Pb isotopic variation and terrestrial disturbance, no samples of this study produced useful age information; however the clear divergence from the previously assumed 238U/235U of any troilite in Muonionalusta introduces substantial uncertainty to the previously reported absolute age of the sample without knowledge of the 238U/235U of the sample.Uncertainties associated with U isotope heterogeneity do not allow for definition of a robust age of solidification and cooling for the IVA core. However, one sample of this work—paired with previous work using short-lived radionuclides—suggests that the cooling age of the IVA core may be significantly younger than previously thought. This work indicates the metallic cores of protoplanetary bodies solidified no earlier than the first ∼5–10 million years of the Solar System.

Solar Wind Plasma Interaction with Asteroid 16 Psyche: Implication for Formation Theories

AbstractThe asteroid 16 Psyche is a primitive metal‐rich asteroid that has not yet been visited by spacecraft. Based on remote observations, Psyche is most likely composed of iron and nickel metal; however, the history of its formation and solidification is still unknown. If Psyche is a remnant core of a differentiated planetesimal exposed by collisions, it opens a unique window toward understanding the cores of the terrestrial bodies, including the Earth and Mercury. If not, it is perhaps a reaccreted rubble pile that has never melted. In the former case, Psyche may have a remanent, dipolar magnetic field; in the latter case, Psyche may have no intrinsic field, but nevertheless would be a conductive object in the solar wind. We use Advanced Modeling Infrastructure in Space Simulation (AMITIS), a three‐dimensional GPU‐based hybrid model of plasma that self‐consistently couples the interior electromagnetic response of Psyche (i.e., magnetic diffusion) to its ambient plasma environment in order to quantify the different interactions under these two cases. The model results provide estimates for the electromagnetic environment of Psyche, showing that the magnetized case and the conductive case present very different signatures in the solar wind. These results have implications for an accurate interpretation of magnetic field observations by NASA's Discovery mission (Psyche mission) to the asteroid 16 Psyche.

Paleomagnetic evidence for dynamo activity driven by inward crystallisation of a metallic asteroid

The direction in which a planetary core solidifies has fundamental implications for the feasibility and nature of dynamo generation. Although Earth's core is outwardly solidifying, the cores of certain smaller planetary bodies have been proposed to inwardly solidify due to their lower central pressures. However, there have been no unambiguous observations of inwardly solidified cores or the relationship between this solidification regime and planetary magnetic activity. To address this gap, we present the results of complimentary paleomagnetic techniques applied to the matrix metal and silicate inclusions within the IVA iron meteorites. This family of meteorites has been suggested to originate from a planetary core that had its overlaying silicate mantle removed by collisions during the early solar system. This process is thought to have produced a molten ball of metal that cooled rapidly and has been proposed to have inwardly solidified. Recent thermal evolution models of such a body predict that it should have generated an intense, multipolar and time-varying dynamo field. This field could have been recorded as a remanent magnetisation in the outer, cool layers of a solid crust on the IVA parent core. We find that the different components in the IVA iron meteorites display a range of paleomagnetic fidelities, depending crucially on the cooling rate of the meteorite. In particular, silicate inclusions in the quickly cooled São João Nepomuceno meteorite are poor paleomagnetic recorders. On the other hand, the matrix metal and some silicate subsamples from the relatively slowly cooled Steinbach meteorite are far better paleomagnetic recorders and provide evidence of an intense (≳100 μT) and directionally varying (exhibiting significant changes on a timescale ≲200 kyr) magnetic field. This is the first demonstration that some iron meteorites record ancient planetary magnetic fields. Furthermore, the observed field intensity, temporal variability and dynamo lifetime are consistent with thermal evolution models of the IVA parent core. Because the acquisition of remanent magnetisation by some IVA iron meteorites require that they cooled below their Curie temperature during the period of dynamo activity, the magnetisation carried by Steinbach also provides strong evidence favouring the inward solidification of its parent core.

Alternative Energy: Production of H2 by Radiolysis of Water in the Rocky Cores of Icy Bodies

Abstract We applied a model of radiolysis in earthly rock–water mixtures to several known or suspected ocean worlds: Enceladus, Ceres, Europa, Titania, Oberon, Pluto, and Charon. In this model, radiation emitted by the long-lived radionuclides (40K, 232Th, 235U, and 238U) contained in the ordinary chondrite-like rocks is partly absorbed by the water permeating the material of each body’s core. The physical and chemical processes that follow release molecular hydrogen (H2), which is a molecule of astrobiological interest. We compared the calculated production of H2 by radiolysis in each body’s core to published estimates of production by serpentinization. This study presents production calculations over 4.5 Gyr for several values of rock porosity. We found that radiolysis can produce H2 quantities equivalent to a few percent of what is estimated from serpentinization. Higher porosity, which is unlikely at the scale of a body’s entire core but possible just under the seafloor, can increase radiolytic production by almost an order of magnitude. The products of water radiolysis also include several oxidants, allowing for production of life-sustaining sulfates. Though previously unrecognized in this capacity, radiolysis in an ocean world’s outer core could be a fundamental agent in generating the chemical energy that could support life.

PLA2G6 accumulates in Lewy bodies in PARK14 and idiopathic Parkinson's disease

The histopathological hallmark of Parkinson's disease (PD) and dementia with Lewy bodies (DLB) is the occurrence of insoluble fibrillary aggregates known as Lewy bodies, in which phosphorylated α-synuclein (α-syn) is a major component. To date, familial PD-linked gene products, including α-syn, parkin, PINK-1, DJ-1 and LRRK2, are known to be involved in Lewy body formation. Phospholipase A2, group VI (PLA2G6) is the causative gene for PARK14-linked parkinsonism (PARK14), a familial form of juvenile-onset dystonia parkinsonism. Several lines of evidence have suggested that PLA2G6 might play a role in the pathogenesis of not only PARK14, but also idiopathic PD. However, no published studies have investigated the association of PLA2G6 with the formation of Lewy bodies. In the present study, we used immunohistochemistry and Western blotting to investigate the involvement of PLA2G6 in Lewy body disease (PD and DLB), multiple system atrophy and Alzheimer's disease, in comparison with normal controls. Although cortical Lewy bodies, which lack a definable central core, were unstained with anti-PLA2G6 antibodies, the cores of brainstem-type Lewy bodies from PARK14 and idiopathic PD patients were moderately or intensely immunopositive for PLA2G6. Our results further reinforce the association of PLA2G6 with the pathogenesis of idiopathic PD, in addition to PARK14.

Tungsten stable isotope compositions of terrestrial samples and meteorites determined by double spike MC-ICPMS

Tungsten stable isotopes hold great potential to examine a variety of physical and chemical processes operating during the accretion and differentiation of asteroids and terrestrial planets, such as core formation and mantle–crust differentiation. To assess the magnitude and origin of W isotope fractionations, we determined the W stable isotopic compositions of six USGS geological reference materials, a NIST steel, and 24 iron meteorites and chondrites. The W isotope data were obtained using multi-collector inductively coupled plasma mass spectrometry (MC-ICPMS) and using a 180W–183W double spike. Chondrites and iron meteorites exhibit a very narrow range in W stable isotope compositions, resulting in a mean δ184/183W=0.027±0.007‰ (95% conf.) relative to the NIST 3163 W standard. This value represents a good estimate for the W stable isotope composition of bulk planetary bodies from the inner solar system. The δ184/183W of some iron meteorites slightly deviates from this value, most likely due to W isotope fractionations induced during crystallization of the metal cores of iron meteorite parent bodies. The investigated terrestrial silicate rocks exhibit a narrow range in δ184/183W, which for most samples is indistinguishable from the mean value of chondrites and iron meteorites. However, felsic samples tend to be isotopically lighter than mafic samples, indicating that magmatic processes on Earth induced W isotope fractionations. These fractionations are possibly related to the fluid-mobility of W in subduction zones, but more data are needed to test this hypothesis. Given that most terrestrial igneous rocks are isotopically indistinguishable from chondrites and iron meteorites, core formation on Earth does not seem to have induced a measurable isotopic fractionation for W. However, more data are needed to firmly arrive at this conclusion.

Elemental partitioning and isotopic fractionation of Zn between metal and silicate and geochemical estimation of the S content of the Earth’s core

Zinc metal–silicate fractionation provides experimental access to the conditions of core formation and Zn has been used to estimate the S contents of the Earth’s core and of the bulk Earth, assuming that they share similar volatility and that Zn was not partitioned into the Earth’s core. Therefore, Zn provides both direct and indirect information into the origin and eventual fate of volatile and siderophile elements on Earth. However, the partitioning of Zn between metal and silicate – as well as the associated isotopic fractionation – is not well known. We have conducted a suite of partitioning experiments to characterize Zn elemental partitioning and isotopic fractionation between metal and silicate as a function of time, temperature, and composition. Experiments were conducted at 2GPa and temperatures from 1473K to 2273K in a piston cylinder apparatus, with run durations from 5 to 240min for four distinct starting materials. Chemical and isotopic equilibrium is achieved within 10min of experimental outset. Zinc metal–silicate isotopic fractionation displays no resolvable dependence on temperature, composition, or oxygen fugacity within the data set. Therefore, the Zn isotopic composition of silicate phases can be used as a proxy for bulk telluric bodies. Partitioning results from this study and data from literature were used to robustly parameterize Zn metal–silicate partitioning as a function of temperature, pressure, and redox state. Using this parametric characterization and viable formation conditions, we have estimated a range of Zn contents in the cores of iron meteorite parent bodies (i.e. iron meteorites) of ∼0.1–150ppm, in good agreement with natural observations. We have also calculated the first geochemical estimates for the Zn contents of the Earth’s core and of the bulk Earth, at 242±107ppm and 114±34ppm (respectively), that consider the slightly siderophile behavior of Zn. These estimates of the Zn contents of the Earth’s core and bulk Earth are significantly higher than previous estimates 0–30ppm and 24–47ppm, respectively. Assuming similar volatility for S and Zn, a chondritic S/Zn ratio, and considering our new estimates, we have calculated a geochemical upper bound for the S content of the Earth’s core of 6.3±1.9wt%. This indicates that S may be a major contributor to the density deficit of the Earth’s core or that the S/Zn ratio for the Earth is non-chondritic.

Iron snow, crystal floats, and inner-core growth: modes of core solidification and implications for dynamos in terrestrial planets and moons

Recent planetary space missions, new experimental data, and advanced numerical techniques have helped to improve our understanding of the deep interiors of the terrestrial planets and moons. In the present review, we summarize recent insights into the state and composition of their iron (Fe)-rich cores, as well as recent findings about the magnetic field evolution of Mercury, the Moon, Mars, and Ganymede. Crystallizing processes in iron-rich cores that differ from the classical Earth case (i.e., Fe snow and iron sulfide (FeS) crystallization) have been identified and found to be important in the cores of terrestrial bodies. The Fe snow regime occurs at pressures lower than that in the Earth’s core on the iron-rich side of the eutectic, where iron freezes first close to the core–mantle boundary rather than in the center. FeS crystallization, instead, occurs on the sulfur-rich side of the eutectic. Depending on the core temperature profile and the pressure range considered, FeS crystallizes either in the core center or close to the core–mantle boundary. The consequences of the various crystallizing mechanisms for core dynamics and magnetic field generation are discussed. For the Moon, revised paleomagnetic data obtained with advanced techniques suggest a peculiar history of its internal dynamo, with an early strong field persisting between 4.25 and 3.5 Ga, and subsequently a much weaker field. In addition, the long-lasting dynamo and the possible presence of an inner core, as inferred from a revised interpretation of Apollo seismic data, suggest core crystallization as a viable process of magnetic field generation for a substantial period during lunar evolution. The present-day magnetic fields of Mercury and Ganymede (if they occur on the iron-rich side of the Fe–FeS eutectic) and the related dynamo action are likely generated in the Fe snow regime and seem to be recent features. An earlier dynamo in Mercury would have been powered differently. For Mercury, MESSENGER data further suggest core formation under reducing conditions that may have resulted in an Fe–S–Si composition, further complicating the core crystallization process. Mars, with its early and strong paleo-field, likely has not yet started to freeze out an inner iron core.