Mapping inner core (IC) seismic anisotropy at high resolution provides important insight on the growth of the inner core through time, its internal dynamics, and its role in the production of the geodynamo. Since the discovery of IC anisotropy (ICA) in 1986, numerous studies have suggested the presence of significant lateral and depth variations in its character and strength. In particular, there is controversial evidence for the presence of a distinct region, spanning the central third of the IC in radius, referred to as the “innermost inner core”. Yet, obtaining robust constraints on the 3D structure of ICA is hampered by the uneven sampling by seismic waves passing through the inner core, and the possible contamination of measurements by unmodelled 3D mantle structure, to which all seismic core phases are sensitive.

Typical ICA models rely on differential travel time measurements between the inner core traversing wave PKPdf (PKIKP) and a reference phase that has a similar path in the mantle, but does not enter the IC (PKPab, PKPbc, PKPcd and related phases). This kind of measurement is thought to minimize mantle contamination, but the global dataset is limited by the distribution of earthquake sources and stations.

Recently, Pham and Tkalcič (2023) devised a clever method to augment the available dataset by including measurements from exotic pairs of core phases that reflect several times at the earth’s surface and repeatedly sample the central part of the inner core, referred to as PKPn. They proposed a new model for ICA and in particular a distinct model for the innermost inner core.

However, we found that their model does not fit the travel time data measured using conventional PKPdf. We investigated the possible cause of this discrepancy by selecting PKPdf measurements on paths sampling similar portions of the mantle as the 16 measurements by Pham and Tkalcič (2023). While some measurements agree, the discrepant data correspond to paths that repeatedly interact with subducted slabs in the mantle.  We thus proceeded to analyse the effects of mantle structure, particularly subducting slabs, on differential travel times of core-sensitive phases. We assessed observed PKPdf and PKPdfn differential times for systematic bias. We find that the higher the “n”, i.e. the greater the number of passages through the mantle, the greater the effect of mantle structure on the PKPdfn measurements, suggesting that the discrepancies between the proposed ICA model constrained by these measurements compared with traditional direct PKP observations are likely due to mantle heterogeneity.

How to cite: Frost, D., Romanowicz, B., and Das, P. P.: Effects of mantle structure on models of seismic anisotropy in the inner core, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-20444, https://doi.org/10.5194/egusphere-egu24-20444, 2024.

Understanding the elastic properties of Earth's inner core is crucial for unraveling its role in the planet’s evolution and dynamics. Seismic shear waves provide a direct means to constrain the shear modulus of the solid inner core at high frequencies. However, their detection has been challenging due to their extremely weak amplitude and interference from other seismic arrivals (Doornbos, 1974). This study aims to provide direct observations of inner-core shear waves through a systematic search using the AlpArray Seismic Network (AASN), a large European seismic array. The approach combines 3-C polarization filtering and slant-stacking techniques. The inspection focuses on events between 2015 and early 2022 within the epicentral distance range of  ~110-150° from the AASN. This source-receiver geometry is close to that of previous PKJKP observation reported using the Gräfenberg array (Cao et al., 2005).

Our systematic search and classification reveal multiple potential observations of PKJKP at frequencies > 0.1 Hz, consistent in both time and slowness with the 1-D Earth model ak135, as well as previous body-wave-based observations, particularly Wookey and Helffrich (2008). The new evidence of PKJKP demonstrates a path forward for formalizing a method for the repeatable detection of inner-core shear waves for different source-receiver geometries. Additional PKJKP observations and comprehensive modeling are essential for gaining insights into the intricate inner-core structure and phenomena, such as anisotropy and focusing effects, which could explain the limited number of observations to date.

How to cite: Ling, O. K. A., Stähler, S. C., and Giardini, D.: Possible Observations of PKJKP in the AlpArray Seismic Dataset, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-18333, https://doi.org/10.5194/egusphere-egu24-18333, 2024.

How to cite: Zhang, F., Yang, H., and Muir, J.: Iron hydride FeHx in the Earth's inner core and its geophysical implications, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-255, https://doi.org/10.5194/egusphere-egu24-255, 2024.

The thermal and electrical conductivities of materials in planetary mantles and cores are crucial for understanding planetary evolution and dynamics. The experimental determination of conductivities at mantle and core pressure-temperature conditions in the diamond anvil cell requires that the sample thickness is precisely known. The standard approach has been to estimate sample thickness from the equations of state of the sample, assuming isotropic contraction (upon compression) or expansion (upon decompression). Recently, however, it has been shown [1] that common pressure media used in diamond anvil cell experiments thin in a strongly non-isotropic manner. If samples embedded in pressure media also deform non-isotropically, then the extant experimental estimates of mantle and core conductivity may contain systematic errors of approximately 30-50% [1]. In situ measurements of sample thickness are needed to verify this inference.

We will report on the first in situ interferometric measurements of Fe foil thickness in a diamond anvil cell with sample configurations resembling that of previous experiments to measure the conductivity of Fe. Our preliminary data show that the contraction and expansion of Fe is strongly non-isotropic, potentially explaining the discrepancies in the reported iron conductivity at core-mantle boundary conditions [2, 3]. We will also discuss practical aspects of future measurements of thermal and electrical conductivity of mantle and core materials in a diamond anvil cell.

[1] Lobanov, S. S., & Geballe, Z. M. (2022). Non-isotropic contraction and expansion of samples in diamond anvil cells: Implications for thermal conductivity at the core-mantle boundary. Geophysical Research Letters, 49, e2022GL100379. [2] Zhang Y., Hou M., Liu G., Zhang C., Prakapenka V.B., Greenberg E., Fei Y., Cohen R. E., and Lin J.-F (2020) Reconciliation of Experiments and Theory on Transport Properties of Iron and the Geodynamo. Phys. Rev. Lett. 125, 078501. [3] Ohta, K., Kuwayama, Y., Hirose, K. et al. (2016). Experimental determination of the electrical resistivity of iron at Earth’s core conditions. Nature 534, 95–98.

How to cite: Breton, H. and Lobanov, S.: In Situ Measurements of Sample Thickness in Diamond Anvil Cells Suggest Large Systematic Errors in High-Pressure Conductivities, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-14702, https://doi.org/10.5194/egusphere-egu24-14702, 2024.

The core of the Earth must have some light elements which are small in concentration but could have dramatic effects on the behavior of the core. Oxygen is one such element. It has long been concluded based on experiments and theoretical calculations (Alfè, Gillan, and Price 2002) that the inner core partitions negligible amounts of O from an enriched outer core and thus its possible effects can be ignored. An oxygen-rich outer and oxygen-poor inner cores has also been proposed as a way to explain various seismic data (Badro, Côté, and Brodholt 2014). The discovery of Fe-O superionic alloys (He et al. 2022) calls these conclusions into questions as the state of O is substantially different at high vs low temperatures which could affect extrapolations of experimental results to high temperatures.

Focusing on the most thermally stable superionic alloys in the inner core, our study systematically investigates the partitioning behaviour of oxygen between solid inner and liquid outer core by an advanced combination of ab initio molecular dynamics (AIMD) simulations and the two-phase thermodynamics (2PT) model (Lin, Blanco, and Goddard 2003). We conclude that while O remains favoured in the liquid state under core conditions non-negligible amounts of O enter the inner core and thus its possible presence cannot be ignored. With realistic concentrations of O in the outer core we produce a density contrast between liquid and solid oxygen that is in the range of that observed at the inner core boundary (ICB) thus showing the importance of obtaining accurate partitioning values and their effect on seismic structure.

This study provides a new and reliable approach to the thermodynamic properties of the superionic state and a new theoretical basis for understanding the internal structure of the Earth's core, contributing to understanding of the complexity of the Earth's interior and providing useful insights into future directions of research in the field of Earth sciences. It also shows the stark difference between high and low temperature structures and how accurate temperatures need to be considered when looking at core structures.

Alfè, D., M. J. Gillan, and G. D. Price. 2002. 'Ab initio chemical potentials of solid and liquid solutions and the chemistry of the Earth’s core', The Journal of Chemical Physics, 116: 7127-36.

Badro, James, Alexander S. Côté, and John P. Brodholt. 2014. 'A seismologically consistent compositional model of Earth’s core', Proceedings of the National Academy of Sciences, 111: 7542-45.

He, Yu, Shichuan Sun, Duck Young Kim, Bo Gyu Jang, Heping Li, and Ho-kwang Mao. 2022. 'Superionic iron alloys and their seismic velocities in Earth’s inner core', Nature, 602: 258-62.

Lin, Shiang-Tai, Mario Blanco, and William A. Goddard. 2003. 'The two-phase model for calculating thermodynamic properties of liquids from molecular dynamics: Validation for the phase diagram of Lennard-Jones fluids', The Journal of Chemical Physics, 119: 11792-805.

How to cite: Chen, Q., Muir, J., and Zhang, F.: Non-negligible Oxygen in the Earth's Inner Core: The importance of high temperatures, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-4505, https://doi.org/10.5194/egusphere-egu24-4505, 2024.

The European XFEL is a new X-ray facility installed near Hamburg, Germany, that provides extremely intense X-ray flashes of less than 50 fs (10^-12 s) that can be repeated every 220 ns (10^-9 s). The facility, coupled with the High Energy Density (HED) instrument, opens new avenues for experiments on iron alloys under planetary core conditions.

The instrument can be coupled with diamond anvil cell experiments. In this case, the X-ray flashes of the XFEL are not only used to measure diffraction images in less that 50 fs, but also to heat the samples and gradually increase sample temperatures every 220 ns, reaching several thousands of degrees at pressures well over a megabar in microseconds. During the 3063 community proposal, we hence tested a new method to explore the phase diagrams of iron alloys at planetary core conditions, inducing phase transformations, melting and microstructural changes in conditions and timeframes that could not be reached in previous experimental systems.

The instrument is also compatible with laser-driven shock experiments. DiPOLE 100-X is a world-class laser that can deliver up to 100 J (in 1-omega) and 50 J (in 2-omega) over up to 15 ns pulses, with a repetition rate up to 10 Hz. It is now installed at the High-Energy Density (HED) beamline of the European XFEL. By shining DIPOLE pulses into polymers in the back of our samples, we can generate pressure and temperature conditions well over 100 GPa and several thousands of K and using the European XFEL, we can get in-situ X-ray diffraction! The facility was tested in May 2023 during the 2740 community proposal, involving over 100 scientists from over 40 world-wide institutions.

In this presentation, I will hence present these new experiments at the European XFEL and preliminary results that can be obtained. These new measurements will require a lot of development and metrology, however, which are actively pursuing at present.

Our work is supported by the ERC HotCores (Grant No 101054994) at the université de Lille.

How to cite: Merkel, S. and Ginestet, H. and the EuXFEL 3063 and 2740 community proposals: New facilities for high pressure / high temperature experiments on iron alloys at planetary core conditions on the European XFEL, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-20584, https://doi.org/10.5194/egusphere-egu24-20584, 2024.

Heat flow mechanisms in terrestrial planetary cores contribute to geophysical processes with broader significance such as the generation of a magnetic field. Thermal convective flow in a planetary core may be found with the combination of adiabatic heat flow estimates—which this study seeks to estimate—and thermal evolution models of total heat flow across the core-mantle boundary. Experimental data constraining the effects of light elements on these processes is still needed. In the case of asteroid Vesta, the core is expected to be composed of Fe alloyed with 13-16wt% S (Steenstra et al., 2019) and 1-2wt% Si (Pringle et al., 2013).

To simulate the conditions of the early Vestan core, the resistivity of Fe alloyed with 16wt% S and 2wt% Si (Fe-16S-2Si) was measured at high pressures and into the liquid state. A 1000-ton cubic anvil press applied a static pressure of 2, 3, 4, or 5 GPa on the sample. The resistivity of Fe-16S-2Si was then calculated from the voltage drop and constant current across the sample at 300-2000 K along with post-experimental geometry measurements.

With the electrical resistivity data, the thermal conductivity of Fe-16S-2Si is estimated using the Wiedemann-Franz Law. For 2-4 GPa, a thermal conductivity of 11+1.5 W/m/K is found. For the top of the core of ancient Vesta, an adiabatic heat flux of 0.3-0.4 mW/m² is derived. These results indicate that the light elements expected in the Vestan core have a large effect on the thermodynamic properties, including more than halving the expected adiabatic heat flow. Since the total heat flux across the early Vestan core-mantle boundary has been previously estimated as >10 mW/m² (Weiss et al., 2010), thermal convection alone may account for the magnetic dynamo in early Vesta with the presence of light alloying elements.

References:

Pringle, E.A., Savage, P.S., Badro, J., Barrat, J.-A., Moynier, F., 2013. Redox state during core formation on asteroid 4-Vesta, Earth and Planetary Science Letters, v. 373, p. 75-82.

Steenstra, E.S., Dankers, D., Berndt, J., Klemme, S., Matveev, S., van Westrenen, W., 2019. Significant depletion of volatile elements in the mantle of asteroid Vesta due to core formation, Icarus, v. 317, p. 669-681.

Weiss, B.P., Gattacceca, J., Stanley, S., Rochette, P., Christensen, U.R., 2010. Paleomagnetic Records of Meteorites and Early Planetesimal Differentiation, Space Science Reviews, v. 152, p. 341-390.

How to cite: Lenhart, E., Yong, W., and Richard, S.: The Adiabatic Heat Flux through the Top of the Core of Ancient Vesta from High-P,T Resistivity Experiments, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-11249, https://doi.org/10.5194/egusphere-egu24-11249, 2024.

Understanding the crystallization of metallic cores is necessary to constrain the structure and thermal evolution of terrestrial bodies in our solar system and beyond. Core cooling is also closely related to the generation and sustainability of a magnetic field. The core crystallization regime depends primarily on the depth of intersection of the core temperature with the liquidus ([1], and refs therein). Core composition, pressure, and thermal profile are the major parameters controlling the depth of intersection. If the temperature gradient across the core is steeper than that of the liquidus, solidification starts at the top, the “top-down” crystallization regime. At low pressure (≤10 GPa) relevant to small terrestrial planets, moons, and possibly some asteroids, the eutectic temperature decreases with increasing pressure (e.g., [2] for the Fe-S system),  favoring  an  onset  of  crystallization  at  the  top  of  the  core. Top-down crystallization has been proposed to exist in several planets and moons in the Solar System, such as Mercury [2], [3], Mars ([4], [5]), and Ganymede [6], [7], [8], [9].

In this study, which was performed by the International Space Science Institute (ISSI) Team “A new non-equilibrium model of iron snow in planetary cores”, we investigate the effect of non-equilibrium as well as the effect of the core composition on top-down crystallization. We find that the time scale of phase relaxation is significantly shorter than the time scales usually employed in one-dimensional evolution models. Consequently, the assumption of equilibrium in these models remains valid. Nevertheless, the time scales associated with crystallization, melting, and crystal settling may be similar to the phase relaxation time scale, which warrants a closer investigation. Additionally, if the amount of supercooling required to initiate nucleation is large [11], non equilibrium could play a much larger role. In terms of core chemistry we studied two different core alloys (Fe-S and Fe-C) motivated by silicate-metal partitioning experiments (reviewed by [12]) at various concentrations in the framework of the equilibrium top-down crystallization model. We find that the time scales of growing either the snow zone (iron-rich compositions) or the flotation crust (iron-poor compositions) can vary significantly between the Fe-S and Fe-C system. Furthermore, the exact concentration of sulfur or carbon has an impact on the thermodynamic parameters, subsequently affecting the entropy available to the dynamo.

References:

[1] Breuer et al., 2015. [2] Chen et  al., 2008. [3] Dumberry & Rivoldini, 2015. [4] Stewart et al., 2007. [5]  Davies & Pommier, 2018. [6] Hauck et al., 2006. [7] Christensen, 2015. [8] Rückriemen et al., 2015. [9] Rückriemen et al., 2018. [10] Loper, 1992. [11] Huguet et al., 2018. [12] Pommier et al., 2022.

How to cite: Rivoldini, A., Rückriemen-Bez, T., Anders, S., Davies, C., Eckert, S., Huguet, L., and Pommier, A.: Top-down crystallization in small planetary bodies: The effect of non-equilibrium and core composition, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-20752, https://doi.org/10.5194/egusphere-egu24-20752, 2024.

The geomagnetic field is sustained by thermochemical convection in Earth’s outer core. Crystallization of the solid inner core releases latent heat and light elements, providing both thermal and chemical buoyancy sources. Most geodynamo simulations use the codensity approach, ignoring the vastly different diffusivities and different boundary conditions for the thermal and chemical fields and thus cannot capture double-diffusive effects. In this study, we consider a numerical convection model of a Boussinesq mixture of light elements in a heavy fluid confined within a rotating spherical shell. The governing parameters are the Ekman number (𝐸 = 2 × 10⁻⁵), a non-dimensional measure of the rotation rate, the thermal and chemical flux Rayleigh numbers (𝑅𝑎_𝑇 = 9 × 10⁶ − 1.2 × 10⁸ and 𝑅𝑎_𝜉 = 3 × 10⁶ − 5 × 10¹⁰), representing the non-dimensional thermal and chemical forcing, and the thermal and chemical Prandtl numbers (𝑃𝑟_𝑇 = 1 and 𝑃𝑟_𝜉 = 10), that are fluid properties. We have performed a detailed analysis of the force balance that emerges within these simulations. We find a transition from a thermal wind to a chemical wind balance with increasing chemical forcing in the azimuthally averaged ”mean” forces in the radial direction. The transition is found to occur at buoyancy ratio, Λ = (𝑅𝑎_𝑇 /𝑃𝑟_𝑇 )/(𝑅𝑎_𝜉 /𝑃𝑟_𝜉 ) ≃ 1. However, the corresponding ”fluctuating” balance is quasi-geostrophic in all directions. The analysis lets us locate the geophysically relevant ”rapidly rotating” regime in this parameter space.

We proceed by imposing a laterally heterogeneous thermal flux at the core-mantle boundary (CMB) in our rapidly rotating double-diffusive simulations. Recent thermally-driven simulations with lateral variations in CMB heat flux produce local regions with a subadiabatic thermal gradient near the CMB (Mound et al., 2019), termed as regional inversion lenses (RILs). This may reconcile the conflicting inferences about the possibility of a globally stratified layer at the top of the core (Kaneshima 2018; Gastine et al. 2020), by accommodating the possibility of both stable and unstable regions. Our goal is to assess the effect of chemical buoyancy on the RILs. The parameter space now also includes the pattern and amplitude of lateral variation in the CMB heat flux. A standard ’tomographic’ pattern, as suggested by seismic measurements (Masters et al., 1996), has been used in these simulations. The amplitude is characterized as 𝑞^∗ = (𝑞_𝑚𝑎𝑥 − 𝑞_𝑚𝑖𝑛)/𝑞_𝑎𝑣𝑔 where 𝑞_𝑚𝑎𝑥, 𝑞_𝑚𝑖𝑛, and 𝑞_𝑎𝑣𝑔 are the maximum, minimum and horizontally averaged heat flux through the CMB. We study the RILs by varying the lateral heterogeneity with 𝑞∗ = {1, 2.3, 5} and buoyancy ratios with Λ = 400-0.01. These RILs are characterized by their strength, measured by a characteristic Brunt-Väisälä frequency (𝑁). Their thickness (𝐿) is measured as the distance of the point of neutral stability from CMB, and the chemical anomaly (𝛿𝜉 ) represents the difference in chemical composition across the lenses. The scaling dependence of these quantities (Mound & Davies, 2020) on the chemical forcing has been explored to extrapolate their values for Earth-like parameters.

How to cite: Naskar, S., Mound, J., Davies, C., and Clarke, A.: Top-heavy double-diffusive convection with core-mantle boundary heat flux variations, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-289, https://doi.org/10.5194/egusphere-egu24-289, 2024.

Near the equatorial region of the Earth’s core, secular variation in the geomagnetic field consists of short period fluctuations. Such fluctuations in the magnetic field are believed to be the result of equatorially trapped waves close to the core-mantle boundary. The balance between the magnetic, Coriolis and buoyancy forces can sustain waves if a stably stratified layer exists in the outermost regions of the core. In this study, a shallow water model with additional magnetic field effects has been used to investigate the characteristics of such equatorially trapped waves. A two-layer model is studied analytically to investigate the effects of radially varying background magnetic fields on the equatorially confined MAC waves. Dispersion relations obtained are significantly influenced by the dependency of the second layer pressure gradient on that of the first layer.  Moreover, the reduced gravity effects in the second layer also modifies the second layer dynamics. Additional parameters, formulated in terms of density, magnetic field strength and buoyancy frequency of both layers characterize the system. The modified properties of a two layer model compared to a single layer is investigated for various regimes of such control parameters. It is found that the alteration in the second layer’s buoyancy frequency significantly influences the dynamics of the MAC (Magnetic-Archimedes-Gravity) wave.

How to cite: Sharma, D. K. and Sahoo, S.: Equatorially trapped waves in a stratified region in the Earth’s outer core modeled using 2-layer shallow water equations, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-2692, https://doi.org/10.5194/egusphere-egu24-2692, 2024.

A significant portion of the Earth’s observed magnetic field is sustained by fluid motion in the planet’s outer core (geodynamo) and varies over time. Records of the past magnetic field come from a variety of sources including, paleo- and archaeomagnetic data. In the modern era, satellite-based observations from missions such as SWARM, have led to a new level of spatial and temporal resolution in our knowledge of the magnetic field. Such observations of the field’s secular variation (SV) can provide a unique window into the deep interior of the Earth. However, understanding the origins and implications of observed SV calls for connecting data to models of Earth’s core dynamics.

Over the last 10-15 years, there has been increasing interest in using data assimilation (DA) to connect numerical dynamo simulations with magnetic field observations. DA is a general term for methods by which one can produce a “weighted combination” of numerical models and observations, to estimate a system’s overall state. This approach is widely used in applications such as numerical weather prediction, where DA is used to, for example, determine initial conditions for forecasts.

We present recent work in the development of DA as a tool for understanding the Earth’s deep interior, using NASA’s Geomagnetic Ensemble Modeling System (GEMS). In simple terms, we “nudge” an ensemble of numerical geodynamo model runs toward observed magnetic field variations according to an Ensemble Kalman Filter (EnKF) framework. This process has the potential to recover information about dynamics which cannot be directly observed, such as the fluid flow and magnetic field deep within the interior. We highlight recently improved capabilities of GEMS, investigate its ability to constrain the core state, and discuss the impact of SWARM data on this work.

How to cite: Gwirtz, K., Kuang, W., and Sabaka, T.: Estimating core dynamics via the assimilation of magnetic field models into numerical dynamos, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-3649, https://doi.org/10.5194/egusphere-egu24-3649, 2024.

The origin of the Earth's and planetary magnetic field is thought to arise from the convective flow of conducting liquid metal, particularly iron, in the deep interior of planetary systems through dynamo action. In numerical simulations, the nature of the resulting magnetic field depends on the imposition of buoyancy profiles that drive convection. Additional influence of imposed magnetic field on convective flows have been studied to understand the back reaction of dynamo action on fluid flow. In the present study, onset of  magnetoconvection is investigated to understand the physical effects in polar regions of the Earth's core where buoyancy forces exhibit a substantial component along the rotation axis. A simplified plane layer convection setup has been used to investigate the fundamental physical mechanisms. Various strengths of uniform magnetic fields in both horizontal and vertical directions have been incorporated. The novel aspect of the study is the incorporation of thermally stable layers with weak and strong stratification. Imposition of thermally stable stratification reduces the threshold of convective instability. It also restricts heat transport to unstable regions only. However, rapid rotation favors penetration of axial velocity into the thermally stable region, although critical thermal forcing for initiating convection also increases. The spectral characteristics of the flow is significantly modified due to the imposition of a stable stratified layer with background uniform magnetic field.

How to cite: Barman, T., Das, A., and Sahoo, S.: Back reaction of magnetic field on rotating penetrative convection, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-3475, https://doi.org/10.5194/egusphere-egu24-3475, 2024.

How to cite: Giraud, V., Noir, J., Burmann, F., and Cébron, D.: Numerical and experimental investigation on the effect of topography on the hydrodynamics of planetary fluid envelops., EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-7843, https://doi.org/10.5194/egusphere-egu24-7843, 2024.

How to cite: Mandea, M., Dehant, V., and Cazenave, A.: Probing the deep Earth interior by a synergistic use of magnetic and gravity fields, and Earth's rotation  , EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-3539, https://doi.org/10.5194/egusphere-egu24-3539, 2024.