Given its unusually high bulk density, Mercury represents a world unique among other terrestrial planets in the solar system. While the general aspects of its interior, such as the core size, are relatively well constrained by the measurements of the planet mass, radius, and moments of inertia, details of its mantle viscosity and thermal profile are still relatively unknown. Recent estimates of Mercury‘s tidal Love number k₂, along with a surprisingly low moment of inertia factor (MoIF) obtained from the MESSENGER gravity data [1] indicate a weak mantle with a CMB viscosity potentially as low as 10¹³ Pa s [2, 3]. Alternative estimates of Mercury‘s MoIF based on laser altimetry (e.g., [4]) would allow a higher CMB viscosity [2] but were reported by [3] as only marginally consistent with the newest value of k₂ from [1].

In this work, I construct interior models of Mercury constrained by a set of geodetic observables including the mean density, polar MoIF, relative moment of inertia of the mantle, and the tidal Love numbers k₂ and h₂. The acceptable interiors are seeked by means of Bayesian inversion. The core is modelled as an Fe-Si-C-S alloy [5] and the mantle is either considered homogeneous (Case A) or endowed with two possible bulk chemical compositions (Case B), derived from the composition of surface lavas [6, 7]. The density and elastic properties of the mantle in Case B are calculated with the thermodynamic software Perple_X [8]. At the CMB, I prescribe a distinct layer, which might either correspond to crystallised Fe-S at the top of the core or to a denser material at the base of the mantle (see also [9]). For the constraining MoIF, I choose the laser altimetry-derived value [4] in one set of samples and the gravity-derived value [1] in the second set of samples.

The presence of a distinct CMB layer with homogeneous fitted properties (density, viscosity) alleviates the need for a weak mantle. While the CMB layer’s viscosity tends to values below 10¹⁸ Pa s, the posterior probability distribution of the lower-mantle viscosity peaks above 10²⁰ Pa s. Moreover, the models from Case B tend to prefer higher values of MoIF~0.34 and cannot be easily reconciled with the lower gravity-derived estimate. In the inversion with laser altimetry-derived MoIF, the CMB layer is predicted to have thickness between 40-160 km and a wide range of possible densities. Outer radius of the liquid part of the core peaks around 1990 km and the temperature above the CMB layer is typically below 1600 K. Silicon content in the outer core peaks around 7 wt%, while sulfur and carbon represent a minor component (2-3 wt%).

[1] Genova et al. (2019), doi:10.1029/2018GL081135.

[2] Steinbrügge et al (2021), doi:10.1029/2020GL089895.

[3] Goossens et al. (2022), doi:10.3847/PSJ/ac4bb8.

[4] Bertone et al. (2021), doi:10.1029/2020JE006683.

[5] Knibbe et al. (2021), doi:10.1029/2020JE006651.

[6] Namur et al. (2016), doi:10.1016/j.epsl.2016.01.030.

[7] Nittler et al. (2018), doi:10.1017/9781316650684.003.

[8] Connolly (2009), doi:10.1029/2009GC002540.

[9] Hauck et al. (2013), doi:10.1002/jgre.20091.

How to cite: Walterova, M.: The interior structure of Mercury constrained by geodetic data, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-3557, https://doi.org/10.5194/egusphere-egu26-3557, 2026.

Mercury will soon be visited by the BepiColombo mission, whose scientific objectives span a wide range of topics in physics and planetary science. Investigating its interior and origin is crucial for understanding the formation and evolution of the Solar System. To this aim, the Mercury Orbiter Radio science Experiment (MORE) will enable the determination of the static gravity field and Mercury’s potential Love number k₂, which quantifies the response of a planetary body’s gravity potential to tidal forcing.

In many studies, a static tide approximation is adopted, leading to the determination of a single k₂ value. This approach is appropriate when the planet is treated as purely elastic, so that the tidal response is instantaneous and in phase with the tidal forcing. A more physically consistent description of the interior, however, requires viscoelastic rheologies, which induce a lag in the tidal response. Under these conditions, the static tide approximation is more adequate when the orbit is circular and the planet is in synchronous rotation (tidally locked). Mercury, however, is in a 3:2 spin-orbit resonance and has an eccentric orbit (e = 0.2056), making a dynamical tide description required. To implement it, the tidal potential is expanded as a Fourier series over multiple tidal modes. The main consequence of this approach is the emergence of a frequency-dependent Love number, k₂(Ιω_2mpqΙ) , evaluated at the specific forcing frequencies Ιω_2mpqΙ.

The aim of this work is to investigate the scientific insights that could be gained from measuring k₂(Ιω_2mpqΙ). Since not all tidal modes contribute equally, we focus on those expected to account for the largest fraction to the tidal signal. We then consider different internal models of Mercury and compute the Love numbers associated to the selected modes using ALMA3 and assess their sensitivity to various parameters of the planet’s interior. The main variables examined are the thickness and rigidity of the elastic lithosphere, the size of the liquid outer core, and the viscosity and rheology of the mantle. We demonstrate that the measurement of the dynamical Love number could significantly improve our understanding of Mercury’s mantle relaxation timescales, providing new and essential constraints on its internal structure.

Finally, we performed accurate numerical simulations to verify the feasibility of these measurements with MORE, showing that its sensitivity is adequate to explore the admissible region of the parameter space considered in our models.

How to cite: Consorzi, A., Mitri, G., Durante, D., De Marchi, F., Tartaglia, P., Zurria, A., and Iess, L.:  Unveiling Mercury’s interior with dynamical Love numbers, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-18424, https://doi.org/10.5194/egusphere-egu26-18424, 2026.

The development of hollows on Mercury—small depressions with spectrally bright interiors and halos—may have resulted from the selective loss of volatile components in these regions. Proposed mechanisms driving elemental or molecular volatility include intense solar radiation, micrometeoroid impacts, and repeated thermal cycling, which leave behind a refractory layer with distinct spectral properties. We investigate solar wind ions as a potential darkening agent and demonstrate that Mercury-relevant sulfides preserve their high reflectivity.

Experimental ion-irradiation studies on sulfides such as NiS, CuS, CoS, FeS, and MoS have shown that metallic surface layers can form through cation segregation and preferential sulfur depletion [1–5]. Laboratory work has further revealed iron enrichment at the surface, accompanied by visible darkening, in troilite (FeS) and more recently in pentlandite [(Fe,Ni)₉S₈] subjected to ion and laser irradiation [e.g., 6, 7]. Unlike lunar, meteoritic, and asteroidal materials, which contain significant iron and nickel sulfide minerals, Mercury’s surface appears depleted in iron. Instead, sulfides are expected to be dominated by Mn, Ti, Cr, Mg, and Ca cations, based on correlations with sulfur detected by MESSENGER’s spectrometer suite [8–10].

We have previously shown that the sulfides: niningerite (MgS) and oldhamite (CaS), two phases proposed as likely hollow-forming material based on visible-to-near-infrared (VNIR) spectral analysis [11], are radiation-hard [12]. These sulfides thereby resist the formation of a metallic top layer, observed in ion-irradiated Fe-sulfides, when exposed to solar wind-speed protons and helium ions.

Subsequent spectral analysis of the irradiated CaS and MgS showed brightening in parts of the visible range (0.4-0.7 µm) of the VNIR (Fig. 1) and an overall brightening in the mid-infrared (MIR) range observed by BepiColombo (7-14 µm, Fig. 2). The sample labeled as oxidized was exposed to air for months after the experiments, which led to an overall darkening in both VNIR and MIR, erasing the effect of irradiation. On Mercury, there is no immediate oxidation of the top layer; instead, re-deposition of thermal and ion desorbed material introduces surface contaminants, which over geological timespans could form a layer. The radiation-hard nature of sulfides could thereby act as a cleaning mechanism, where contaminants are removed continuously under solar wind exposure without damaging the bulk, preserving the reflectivity of the sample. This process provides a new framework for understanding the formation of bright hollow materials, highlighting the importance of non-transition-metal sulfides in Mercury’s surface evolution.

Figure 1: Visual-to-near infrared measurement of fresh MgS (black line) compared to 2 keV protons (salmon) and an old, oxidized sample (yellow). Two unirradiated MgS samples are shown, whereas one is fresh (syn) and one is old and oxidized (old).

Figure 2: Mid-infrared measurements of two MgS samples sourced from BenchChem (BC, solid lines) and Zegen Metals & Chemicals (ZMC, dashed lines). The irradiated samples (light gray) have a consistently higher reflectivity than the unirradiated (fresh) samples. The heavily oxidized sample (yellow) is the darkest.

How to cite: Jäggi, N., Barraud, O., and Dukes, C.: Self-cleaning Sulfides as Mercury Hollow Bright Material, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-5210, https://doi.org/10.5194/egusphere-egu26-5210, 2026.

The knowledge of Mercury's crater record has significantly evolved during the last decade thanks to the MESSENGER mission, which enabled the implementation of updated global crater catalogs by allowing the identification of a wealth of previously unknown impact structures. Particularly, recent re-examination of MESSENGER data led to the identification of tens of previously unreported large (D>150 km) impact basins. These large basins have not yet been studied in detail despite their significant geological and geophysical importance. Here, we present geological, topographical, structural, compositional, and geophysical investigations of one (maybe the largest) of these basins. The basin has not yet an International Astronomical Union (IAU) name but it has been reported as b56 or Lennon-Picasso basin in the published literature. The basin has an approximate diameter of more than 1500 kilometers and is centered at about 15S, 50E, located north-westward of Rembrandt basin. However, the most external structures associated to this basin extend fairly more than 1500-km form its center, suggesting a diameter closer if not higher than 2000 km, thus equivalent if not bigger than Caloris basin, known as the largest Mercury’s basin. Geology, tectonics, and composition of this basin have been investigated by using photointerpretation and remote sensing techniques applied to all the available data. Visible imagery from MDIS camera has been integrated with Digital Elevation Models (DEM), spectral data (color mosaics and data from MASCS), and gravity data from the Radio Science (RS) experiment onboard of MESSENGER into Geographic Information System (GIS) environment. DEM and slope maps highlight the annular terraced floor of the basin, suggesting that this may have formed as a peak ring or multiring structure. The basin is defined by several major lineaments (up to thousands of km long) consisting of a series of tectonic structures encompassing a broadly circular topographic low corresponding to the internal floor of the basin. This central region shows a gravity anomaly and a low crustal thickness with respect to the surrounding areas. The impact triggered volcanic activity since the floor presents the typical characteristics of other volcanic infilled Mercury’s basins: a smoother texture and lower albedo with respect to the surroundings regions, radial faults, wrinkle ridges and concentric circular lobate scarps, and spectral signatures from MASCS data. Most importantly, our results show that the tectonics associated to this basin, along as that of many other recently discovered large basins, might have had a regional and global significance, which has been so far overlooked. Indeed, these impact-related structures have been so far included in current estimates of Mercury’s contraction, most likely leading to its overestimation. After presenting the above mentioned lines of evidence we will discuss the implications of the tectonics of Mercury’s large basins for the planet global tectonics and contraction estimates.

How to cite: Di Achille, G., D'Incecco, P., and Caddeo, Y.: Don’t call it b56: geology and geophysics of a Caloris-size impact basin and implications for Mercury’s global tectonics, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-21371, https://doi.org/10.5194/egusphere-egu26-21371, 2026.

The MERTIS (Mercury Radiometer and Thermal Infrared Spectrometer) instrument aboard the ESA–JAXA BepiColombo mission is designed to characterize Mercury’s surface mineralogy using thermal infrared spectroscopy in the 7-14 µm range [1,2]. During BepiColombo’s fifth Mercury flyby on 1 December 2024, MERTIS acquired the first spatially resolved mid-infrared spectra of Mercury’s surface, collecting more than 1.4 million spectra at spatial resolutions of approximately 26–30 km per pixel [3,4]. These observations revealed spectral variations associated with impact craters, bright and dark deposits, and other geological features, providing an important preview of the global dataset that will be obtained after Mercury orbit insertion in late 2026.

However, interpreting thermal infrared spectra of Mercury is challenging due to the planet’s extreme surface temperatures (~100–700 K) and strong thermal gradients, which produce non-isothermal conditions within individual MERTIS pixels. These conditions obscure mineralogical features by blending them with multiple temperature-dependent Planck radiation, making accurate determination of the emissivity a central challenge [1,5,6]. In addition, thermal infrared spectral features are influenced by physical surface properties such as grain size, porosity and surface roughness, further increasing interpretation uncertainties [7,8,9]. Robust analysis of the upcoming global MERTIS dataset therefore requires laboratory reference measurements under comparable conditions.

To support ongoing laboratory studies, we developed the MERTIS Imaging Model for Instrument Characterization (MIMIC), a dedicated laboratory emulator that reproduces the imaging geometry and spectral behavior of MERTIS. MIMIC is designed as a complementary approach to established bulk emissivity measurements acquired with Fourier-transform infrared (FTIR) spectroscopy, extending these methods by enabling spatially resolved thermal infrared imaging under Mercury-like thermal conditions at DLR’s Planetary Spectroscopy Laboratory (PSL). Through a mid-infrared transparent window mounted on a high-temperature, evacuated emissivity chamber, MIMIC produces imaging data that are comparable to MERTIS observations. This capability allows systematic investigation of how surface physical properties, such as grain size, grain shape (angularity and sphericity), porosity, and surface roughness, affect thermal emission at the pixel scale. By bridging laboratory spectroscopy with orbital observations, MIMIC offers a unique platform to improve the interpretation of MERTIS data and our understanding of mid-IR emission processes on airless planetary bodies.

[1] Hiesinger, H., et al., 2010, Planetary and Space Science [2] Helbert, J., et al., 2013, SPIE [3] Hiesinger, H., et al., 2025, LPSC [4] Adeli, S., et al., 2025, EPSC-DPS [5] Wohlfarth, K., et al., 2023, Astronomy & Astrophysics [6] Tenthoff, M., et al., 2025, EPSC-DPS [7] Maturilli, A., et al., 2006, Planetary and Space Science [8] Morlok, A., et al., 2016, Icarus [9] Martin, A.C., et al., 2025, JGR Planets

How to cite: Domac, A., Adeli, S., Helbert, J., Althaus, C., Maturilli, A., D'Amore, M., Barraud, O., Garland, S., Knollenberg, J., Walter, I., Verma, N., Van der Neucker, A., Alemanno, G., Lorek, A., Hamann, C., Wünnemann, K., and Hiesinger, H.: A Laboratory Imaging Emulator for the MERTIS Instrument in preparation for BepiColombo Mission: MIMIC, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-20040, https://doi.org/10.5194/egusphere-egu26-20040, 2026.

The ESA-JAXA joint mission BepiColombo is still on the track to Mercury and will be inserted into Mercury orbit in November 2026. It completed all flybys by January 2025 and conducted numerous scientific observations. The Mercury Transfer Module will be first separated in September 2026, followed by insertion into Mercury's orbit in November 2026. Subsequently, the Mercury Magnetospheric Orbiter (Mio) will separate in December 2026, deploying its wire antennas and magnetometer masts. Following initial checkout of the spacecraft bus and scientific instruments, along with test observations, the nominal science phase will start in April 2027. The baseline observation plans for Mio faces thermal constraints during the perihelion season and power constraints during the aphelion season, respectively. Operation planning and updating is progressing to address these limitations. This presentation will report on the latest status of BepiColombo/Mio and its upcoming operation and observation plans.

How to cite: Murakami, G., Jones, G., and Besse, S.: Updates and upcoming operation plans of BepiColombo/Mio, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-16269, https://doi.org/10.5194/egusphere-egu26-16269, 2026.

Because of Mercury’s close orbital position to the Sun and its low mass, the planet cannot retain a dense atmosphere and instead possesses an exosphere. The gaseous species detected so far - such as H, (Mariner 10, MESSENGER), He (Mariner 10, MESSENGER, BepiColombo flyby), (possibly) O (Mariner 10), Na, K, Ca (ground-based and MESSENGER), Mg (MESSENGER), and Li and H₂ (inferred from MESSENGER magnetic field data) - yield a column content in the order of about 10¹² cm⁻², which is lower than the expected column content of an exosphere which is in the order of about 10¹⁴ cm⁻². In addition to these elements, MESSENGER’s FIPS instrument also detected C, OH, H₂O, Ne, Al, Si, O₂, Ar, CO₂, Ti, and Fe ions at the downstream of Mercury. Atmospheric measurements from the Mariner 10 occultation experiment indicate that the electron density near the planet's surface is less than 10³ cm^-3 on both sides of the planet, implying an upper limit to the dayside surface gas number density of about 10⁶ cm^-3. The observed elements are expected to represent only a small fraction of Mercury’s exosphere,  as the total surface pressure contributed by these known species is far lower than the upper limit for the exospheric surface pressure of 10^-11 - 10^-12 bar. While H and He appear to originate from the solar wind (i.e., thermal release of implanted solar wind ions), heavier elements are sourced from the planet’s regolith and may be delivered by meteoroids of various sizes. In this study, we investigate the role of meteoroids and their contribution to the elemental input on Mercury's surface and exosphere. We also discuss the potential effects of meteoritic material on the volatile components of the planet's surface composition and examine which currently undetected elements, potentially delivered from meteoroids, may contribute to the still-unknown surface pressure.

How to cite: Lammer, H., Weichbold, F., Scherf, M., Schmid, D., Berezhnoy, A., Varsani, A., and Volwerk, M.: The role of meteoritic delivery to Mercury’s surface-exosphere environment, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-18943, https://doi.org/10.5194/egusphere-egu26-18943, 2026.

Mercury’s exosphere has been extensively investigated through ground-based observations. Since 2007, the THEMIS solar telescope was used to conduct a long-term monitoring campaign of the sodium (Na) exosphere, enabling detailed studies of its morphology and variability at different timescales driven by interactions between Mercury’s surface, intrinsic magnetic field, neutral and ionized environment, and the solar wind and radiation. They allowed to investigate the contribution of the different source processes as well as the statistical frequency of the different morphological patterns, and the rapid change from one to another at the sudden change of interplanetary magnetic field conditions.

In 2022, 2023, and 2024, we carried out targeted observations of Mercury’s sodium exosphere in the days surrounding three of the six flybys performed by the ESA–JAXA BepiColombo spacecraft around the planet. The objective was to provide a global view of the exospheric morphology and dynamics during the spacecraft’s close-approach phase, when also several in-situ instruments were simultaneously operating. These measurements offered crucial information on the planetary environment, including magnetic fields, as well as ion, electron, and neutral populations across a wide range of energies, and radiation.

We present and compare the three exospheric configurations observed in the days around these three flybys, highlighting their morphological and dynamical similarities and differences.

How to cite: Mangano, V., Leblanc, F., Del Moro, D., Milillo, A., Moroni, M., Gelly, B., Douet, R., Laforge, D., and Zender, J.: The Exosphere of Mercury during BepiColombo's Flybys 2, 3, and 4, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-14265, https://doi.org/10.5194/egusphere-egu26-14265, 2026.

Mercury hosts a small global magnetic field, approximately 1% of Earth’s magnetic field strength, capable of standing off the solar wind, resulting in a magnetosphere that is qualitatively similar in structure to Earth’s. However, due to its closer proximity to the Sun, Mercury’s magnetosphere experiences much stronger solar wind pressure than that at Earth, resulting in dynamic magnetospheric processes that occur on much shorter timescales. These extreme conditions can result in processes such as particle energization, transport and precipitation onto the planetary surface, which are strongly influenced by the external solar wind conditions. Here, we present observations of energetic protons (> ~ 1 MeV) and electrons (> ~ 70 keV) from the Solar Intensity X-Ray and Particle Spectrometer (SIXS) onboard the BepiColombo spacecraft during its sixth and final Mercury flyby on 8 January 2025. Similar to the spacecraft’s fourth Mercury flyby in 2024, a solar energetic particle event occurred a few days before closest approach, resulting in elevated fluxes of energetic particles both outside and within the Hermean magnetosphere. Furthermore, the KTH22 Mercury magnetic field model was used to help interpret these energetic particle observations and to evaluate whether features in the data were consistent with the aforementioned magnetospheric processes.

How to cite: Edwards, L., Grande, M., Lawrence, D., Vainio, R., Aizawa, S., Hadid, L., Raines, J., Lehtolainen, A., Esko, E., and Kilpua, E.: Energetic Particle Observations with SIXS During BepiColombo’s Sixth Mercury Flyby, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-7327, https://doi.org/10.5194/egusphere-egu26-7327, 2026.

We present global modelling of Mercury’s solar wind interaction with the open-source 3D hybrid-particle code framework RHybrid (paRallel Hybrid) in light of BepiColombo's flybys and forthcoming orbital science observations. In the hybrid-particle model, ions are treated kinetically as macroscopic particle clouds (macroparticles) moving under the Lorentz force, while electrons are described implicitly as a charge-neutralising, inertialess fluid governed by Ohm’s law. The kinetic ion dynamics are coupled to the evolution of the magnetic field through Faraday’s law, and the system is closed using Ampère’s law. This approach allows ion velocity distributions to evolve self-consistently, capturing wave-particle interactions, finite Larmor radius effects, and other ion-kinetic processes. The code is highly parallelised using message passing between compute nodes, enabling efficient use of large high-performance computing resources. This allows us to simulate spatial structures and ion velocity distributions in the Hermean plasma environment with high resolution, resolving the coupling between ion scales and global magnetospheric scales.

In the model, Mercury’s surface is represented as a particle-absorbing boundary, with the underlying crust–mantle region modelled as a resistive spherical shell overlying an ideally conducting core. The intrinsic planetary magnetic field is prescribed as a dipole offset northward from the planet’s centre, or alternatively by any other 3D planetary magnetic field model. The production of exospheric ion species is described through photoionisation of arbitrary 3D neutral density profiles.

Here we discuss the application of global hybrid modelling to study the formation, structure, and dynamics of different regions in the Hermean plasma environment, as well as ongoing development of the RHybrid code, including adaptive mesh refinement, temporal substepping, and improved electron physics. Mercury’s environment is characterised by strong couplings and feedbacks between the solar wind, magnetosphere, exosphere, surface, mantle, and core. Global hybrid modelling provides essential context for interpreting in situ observations, enables controlled numerical experiments under varying conditions, and supports systematic and flexible investigations of the scaling of solar wind interaction processes.

How to cite: Jarvinen, R., Honkonen, I., Kallio, E., Phillips, D., Dubyagin, S., Grant, S., and Borg, M.: Interpreting BepiColombo's observations of Mercury's solar wind interaction with global hybrid-particle simulations, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-19073, https://doi.org/10.5194/egusphere-egu26-19073, 2026.

Planetary magnetospheres are elaborate systems of internal and external factors, ranging from the internal planetary magnetic moment and currents in the magnetospheric boundaries to exosper-ionosphere-surface interaction, and variation in solar wind properties.
In general, these flows and fields are usually interacting non-linearly.
However, there are regions in the magnetosphere where properties may be understood in terms of a linear superposition.
Here, we investigate the far downtail regions of the nightside magnetotail, where two key factors are the compressed but decreasing planetary magnetic field and the surrounding interplanetary magnetic field (IMF).

Thus, we conduct 12 global model runs of Mercury's magnetosphere with 6 IMF directions in Cardinal and Parker Spiral directions each.
We then superimpose 3 Cardinal IMF runs to emulate linear combined Parker Spiral (LC) IMF cases and compare these to the real Parker Spiral IMF case runs along the downtail passages of the MPO and Mio spacecraft of the BepiColombo mission.
It is found that most LC cases share a surprising level of similarity with the real IMF cases for features such as the general tail twist, suggesting that some physical processes within the magnetotail may be described as linear, despite the overall interaction is non-linear.
Finally, we further investigate approaches to the definition of a threshold of linearity.

How to cite: Exner, W. and Romanelli, N.: On the Linearity of Mercury's Nightside Magnetosphere, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-11061, https://doi.org/10.5194/egusphere-egu26-11061, 2026.

Most global simulations of Mercury’s magnetosphere assume a steady solar wind. However, the planet's extremely small magnetosphere responds on characteristic timescales of only a few minutes, making it inherently sensitive to solar-wind variability. Such rapid temporal forcing is expected to generate a highly dynamic magnetospheric environment, favorable to the development of plasma instabilities. These processes can facilitate electron entry into the magnetosphere, their subsequent trapping and acceleration and, in some cases, their direct interaction with Mercury’s exosphere and surface.

To investigate these effects, we perform global magnetohydrodynamic (MHD) simulations of Mercury’s magnetospheric response to both steady and time-dependent solar-wind conditions using the spherical code PLANET_MAG_AMRVAC. These simulations are designed to support the upcoming science phase of the BepiColombo mission, scheduled to begin in less than a year, by predicting magnetospheric and exospheric observables accessible to instruments onboard both Mio and MPO under a broad range of solar-wind conditions.

As a first step, the model was tested through comparisons with electron density measurements obtained by the MEA1 instrument onboard Mio during Mercury’s three firsts flybys. The simulations include a planetary plasma source driven by the photoionization of exospheric neutrals, allowing for a more realistic representation of plasma populations in Mercury’s near-planet environment. In parallel, the code was used to predict the quasi-thermal noise spectra measurable by the SORBET instrument during flybys, when the antennas cannot be fully deployed during the cruise phase.

Building on this foundation, the focus of this work is the impact of transient solar wind structures -- for now magnetic holes or vortices -- on Mercury’s magnetosphere. Particular attention is paid to their transmission through the bow shock, their evolution within the magnetosheath, and the conditions under which they can penetrate into the magnetosphere.

To address these questions, we first adopt a global MHD approach to capture the large-scale dynamics and overall morphology of these events. We then aim to confront these results with kinetic or particle-in-cell (PIC) simulations in order to explore the associated small-scale physics beyond the MHD framework. Finally, we outline ongoing and future work involving the injection of test particles, treated within the guiding-center approximation, in selected regions of interest. This approach will allow us to investigate particle transport, acceleration, and loss processes in Mercury’s magnetosphere under different solar-wind disturbance scenarios.

How to cite: Mertz, I., Griton, L., Pantellini, F., Houeibib, A., Issautier, K., Verkampt, B., and Girgis, K.: The dynamic response of Mercury’s magnetosphere to solar wind forcing: consequences for the acceleration of charged particles in a telluric planetary environment, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-17940, https://doi.org/10.5194/egusphere-egu26-17940, 2026.

Mercury hosts a highly dynamic magnetosphere in which energy and momentum can be transported between different regions by field-aligned currents (FACs). The region 1 FAC are generated near the dawnside magnetopause, propagate along magnetic field lines toward the planet, and return toward the dusk magnetospheric flank. In-situ observations have established FACs as a ubiquitous feature of the Hermean magnetosphere. However, in the absence of a substantial ionosphere, the mechanisms by which these currents close remain poorly understood. In this study, we present the analysis results from in-situ MESSENGER magnetic field observations and apply the magnetometric resistivity inversion technique to infer FAC closure pathways above and within the planetary surface and within Mercury’s interior without any pre-assumptions about the conductivity structure. We further show the influence of different inversion side constraints, including solenoidal current continuity and minimum-norm regularization, on the inferred current systems.

How to cite: Heyner, D., Pump, K., Kolhey, P., Plaschke, F., Pommier, A., and Johnson, C.: Magnetometric Resistivity Inversion of Region 1 Field-Aligned Currents in Mercury’s Interior, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-19710, https://doi.org/10.5194/egusphere-egu26-19710, 2026.

The MESSENGER magnetometer data for the years 2012 through 2015 are used to study the presence of mirror modes in Mercury's environment. Using magnetic field only detection of these structures, 10715 intervals of 20 s and longer are found in the solar wind, and in the magnetosheath and magnetosphere of Mercury. The distribution of mirror modes around the planet is similar to that found at Venus and Mars, however, the occurrence rate of 1.0E-4 per second is up to 2 orders of magnitude smaller than at the other two planets. The mirror modes are more prone to be excited near Mercury's aphelion. A comparison shows that mirror modes and magnetic holes have a similar behaviour around Mercury, and that about 40% of the mirror modes can also be identified as magnetic holes. Ion cyclotron waves show a lesser dependence on the true anomaly angle.

How to cite: Volwerk, M., Karlsson, T., Goetz, C., Heyner, D., Plaschke, F., Schmid, D., Simon Wedlund, C., Nakamura, R., Califano, F., Hamrin, M., Pucci, F., Settino, A., and Rojas-Castillo, D.: Mercury's Mirror Modes?, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-5030, https://doi.org/10.5194/egusphere-egu26-5030, 2026.