TP7
This session invites observational, analytical, theoretical, and analogue fieldwork research into any aspect of planetary endogenic processes. We welcome submissions on comparing landforms and processes on multiple bodies; geochemical and chronological data from planetary material; numerical modeling studies; tectonics and seismicity across the Solar System; theoretical and technical designs for current or future missions; as well as data analysis and insights on the seismicity and interior structures of planets and small bodies.
Session assets
Introduction
Current seismic events detected by NASA’s InSight mission suggest that Mars is still seismically and/or tectonically active. Most of the Marsquakes are associated with the Cerberus Fossae region[1,2,3], but the locations of other seismically active centers are poorly constrained [4]. Specifically, recent endogenic activity within Tharsis is poorly constrained although Tharsis-related stresses induced by Late Amazonian volcanic loading[5,6] have likely accumulated within the Martian crust and should lead to recent tectonic activity within this region. To date, only very few morphologically pristine tectonic structures in Tharsis have been documented. Therefore, we followed up on our previous study [7] of the Claritas Fossae region and searched for evidence of recent tectonic structures.
Figure 1 (a) Schematic map of the Tharsis including Thaumasia and Claritas Fossae, our region of interest. Marked by yellow-shaded circles are the positions of proposed source regions of seismic activity of the distant events interpreted for Tharsis [1]. (b) A topographic image of the studied region, the black triangles indicate the locations of investigated fresh-looking scarps. (c) The corresponding topographic profiles of the study region. Produced using the MOLA MEX – HRSC global blended digital elevation model [8].
Observations
The topography of the Claritas Fossae region is dominated by the N020W-trending steep scarp of Claritas Rupes. This scarp, locally exceeding 2,000 meters in height, has been likely formed during the last stage of the main phase of Thaumasia tectonics in the Late Hesperian or Early Amazonian [9]. It was interpreted as the surface expression of a crustal-scale listric normal fault that to the formation of the present regional half-graben morphology [10]. Using the Context Camera (CTX) (5–6 m/px) and High Resolution Imaging Science Experiment (HiRISE) images (25–50 cm/pixel), we identified fresh-appearing scarps with lengths of typically less than one kilometer. Detailed inspection of the scarps reveals uphill-facing (antislope) and pristine morphologies, without evidence of significant modification by erosion or coverage by aeolian deposits. Based on a CTX-based Digital Elevation Model (DEM), we found that the western shoulders of the scarps rise above the inferred average slope of the main scarp, and this topographical offset stops the downslope movement of boulders released from the main Claritas Rupes scarp, leading to their accumulation along the scarps. In some places, where these scarps are not present or less well developed, the boulders were capable of moving further downslope.
Figure 2 (a-b) Examples of identified uphill-facing scarps that stopped and accumulated downslope moving boulders (ESP_078218_1575). (c) Slope map and corresponding CTX-based topographic profile showing that the western shoulders of the scarps rise above the inferred average slope of the main scarp. CTX stereo-pair (P18_007945_1532 and N10_066414_1533) (d) Close-up image of the boulders and their tracks that have been stopped at the antislope scarp (PSP_007945_1555). (e) Schematic drawing presenting the relationship between the uphill-facing scarps and downslope moving boulders (ESP_078508_1555). The north is up.
Discussion and conclusion
The formation of terrestrial uphill-facing scarps is often attributed to Deep-seated Gravitational Spreading Deformations (DGSDs), or instabilities related to glacial retreat. As the studied area does not show any signs of past glaciation(s), neither glacial-induced DGSDs nor post-glacial uplift can readily explain the scarp formation. Uphill-facing scarps could represent antithetic normal faults formed simultaneously or after the formation of the main crustal-scale fault of Claritas Rupes in the Late Hesperian/Early Amazonian [11]. However, this scenario is unlikely due to the pristine morphology of the identified scarps, which argues against such age. Furthermore, their formation could be related to slope gravitational processes such as rotational sliding but we do not find any evidence of the formation of morphologically similar scarps on the other similar-size scarps elsewhere in Tharsis. Nevertheless, the formation of DGSDs can be triggered by the presence of tectonic discontinuities in seismically active regions. Thus, in the context of the long-lived and complex tectonic evolution of the Claritas Fossae region, we infer that that scenario is plausible.
The pristine appearance of the identified scarps suggests that Claritas Fossae might be tectonically inactive. As the determination of absolute (model) ages of small-scale linear tectonic features is almost impossible, we used relative dating. The observed boulders tracks indicate continuous and intense mass wasting processes at the Claritas Rupes scarp that should quickly fill the accommodation space created by the uphill-facing scarps. As a consequence, these small uphill-facing scarps would be covered and precluded from possible identification. Moreover, the pristine appearance of the faults, as visible in image observations and topographic profiles, suggests that the tectonic activity responsible for the fault formation is so young that slope movements and aeolian processes have not yet erased their evidence.
Acknowledgments: BP was financially supported by the Ministry of Education and Science, Poland, with publication grant funding (62.9012.2401.00.0).
References:
[1] Ceylan, S. et al. J. Geophys. Res. Planets 128 (8), e2023JE007826 (2023);[2] Rivas-Dorado, S. et al. Earth Planet. Sci. Lett. 594, 117692 (2022); [3] Horvath, D. G. et al. Icarus 365, 114499 (2021); [4] Stähler, S. C. et al. in 55th Lunar and Planetary Science Conference 2641 (2024); [5] Pieterek, B. et al. Icarus 386, 115151 (2022);[6] Hauber, E. et al. Geophys. Res. Lett. 38, 1–5 (2011); [7] Pieterek, B. et al. 407, 115770 (2024); [8] Balbi, E. et al. Icarus 115972 (2024); [9] Fergason, R. L. et al. US Geol. Surv. (2018) [10] Hauber, E. et al. J. Geophys. Res. Planets 110, 1–13 (2005); [11] Tanaka, K. L. et al. J. Geophys. Res. 93, 893–917 (1988)
How to cite: Pieterek, B., Brož, P., and Hauber, E.: Neotectonic activity at the Claritas Rupes scarp, Thaumasia region, Mars, Europlanet Science Congress 2024, Berlin, Germany, 8–13 Sep 2024, EPSC2024-39, https://doi.org/10.5194/epsc2024-39, 2024.
1. Introduction
The efforts to explore the surfaces of the Moon and Mars are ramping up. Future missions contemplate the construction of permanent base camps [1], which would require a solid knowledge of the terrain and plenty of resources. Understanding the geology of these bodies is of primary importance for this purpose, as well as the identification of potential resource deposits [2]. In this context, medium-scale features gain a bigger relevance, being intrusive domes one of the less investigated [3,4]. Intrusive domes are worth studying, since the geological processes acting over them, and their association with other features like pits and dykes are appealing for space exploration [5].
This abstract showcases the work done in a doctoral research, where we studied two locations: The Valentines domes on the Moon (30.69 N, 10.20 E), and the domes in west Utopia Planitia on in Mars (centred 41°N, and 77°E).
2. Data and Methods
For the Moon, we used a global WAC mosaic, and 23 NAC images from the Lunar Reconnaissance Orbiter [6]. Two DEMs, a global LRO-Kaguya mosaic; and a DEM derived from NAC stereo pairs. We also derived 28 spectral indexes from the Moon Mineralogy Mapper [7]. For Mars, we used the global CTX mosaic, 42 HiRISE images, and 8 CRISM cubes form the Mars reconnaissance Orbiter [8].
To analyse the geological settings of the two locations we used a hybrid mapping approach, incorporating geomorphological and spectral information in a single product [9]. We first created geomorphological units, which were later refined or modified according to the spectral information. We also computed the age of the units using the crater size-frequency counting technique. The analysis and mapping were done in the geoprocessing software QGIS with the aid of Mappy [10].
3. Results and discussion
3.1 MoonIndex
While working with the hyperspectral data of the Moon we noticed the lack of an open-source tool to generate spectral indexes from it, since these are important products to survey the mineralogy of a planetary surface, we developed a Python library called MoonIndex, which recreated 38 indexes from the literature. The workflow of the library can be seen in Figure 1, the processing started with the filtering of the data, followed by the removal of the continuum. The indexes were then calculated following as possible the original formulations. Our results were consistent with the ones in the literature, so they were suitable for interpretation.
Figure 1: Flow-chart of the full procedure of MoonIndex.
3.2 Valentine Domes
After developing MoonIndex, we proceeded with the geostratigraphic mapping of the Valentine Domes (Figure 2). The intrusive domes are oval-shaped structures with low altitude, small slope, and dissected by fractures and faults. We defined three main domes (Ev2, Ev2, Ev3), they have several secondary structures on top of them. These structures were originally classified as kipukas by [3], but a spectral analysis showed that most of them are smaller intrusive domes.
The emplacement of the large domes is related to the intrusion of a large igneous complex below the area, and occurred after 2.8 Ga and before 1.81 Ga. The secondary domes likely formed after 1.81 Ga by intruding dykes. All of this suggest that this system was big and active for several million years, the intrusive rocks might even outcrop thanks to the complex systems of fractures that crosses the domes, which is an opportunity to reach potential resources.
Figure 2: Detailed geostratigraphic map of the Valentine Domes.
3.3 Western Utopia Planitia
This flat region is in the west margin of Utopia Planitia, across the plain are scattered hundreds of monogenetic domes. Due to the large size of the zone, and the small size of the features, our approach consisted of doing a regional mapping of the zone and the detailed mapping of representative domes. Most of the domes are oval-shaped, but others are elongated or have lobes attached to their main body. Most of the domes have an outer crust, which was interpreted by [4] as a mixture of hyaloclastite and periglacial deposits. The domes are likely the product of individual intrusions of a large igneous system beneath the zone, some of them intruded at shallow depths, allowing the formation of the hyaloclastite crust, while others even reached the surface, due to the presence of volcanic craters and lobes. This system is similar to the dome field in Arcadia Planitia [11], both representing a complex system of intrusive-to-extrusive activity.
4. Conclusions
Intrusive domes are uncommon and complex systems in the Moon and Mars, they are usually related with big igneous systems in the subsurface, intensive fracturing, and a mineralogy that contrast with their surroundings, making them interesting location for future exploration.
The hundreds of domes in Utopia Planitia contrast with the three Valentine domes in the Moon, indicating a difference in how these processes occurs in both bodies. Several intrusive domes remain to be discovered and studied, and more research is needed to further characterize their formation and potential use in future missions.
Acknowledgements
This project has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No 101004214.
References
[1] NASA. (2020). NASA’s Lunar Exploration Program Overview.
[2] Lewis et al. (1993). Using resources from neart-earth space.
[3] Wöhler & Lena (2009). Lunar intrusive domes: Morphometric analysis and laccolith modelling.
[4] Farrand et al. (2021). Spectral and geological analyses of domes in western Arcadia Planitia, Mars: Evidence for intrusive alkali-rich volcanism and ice-associated surface features.
[5] Braden & Robinson (2011). Human exploration of the Gruithuisen Domes.
[6] Robinson et al. (2010). Lunar Reconnaissance Orbiter Camera (LROC) Instrument Overview.
[7] Green et al. (2011). The Moon Mineralogy Mapper (M 3 ) imaging spectrometer for lunar science: Instrument description, calibration, on-orbit measurements, science data calibration and on-orbit validation.
[8] Zurek & Smrekar (2007). An overview of the Mars Reconnaissance Orbiter (MRO) science mission.
[9] Aileen Yingst et al. (2023). A Geologic Map of Vesta Produced Using a Hybrid Method for Incorporating Spectroscopic and Morphologic Data.
[10] Penasa, L., & Brandt, C. H. (2021). [Software].
[11] Rampey et al. (2007). Identity and emplacement of domical structures in the western Arcadia Planitia, Mars.
How to cite: Suarez Valencia, J. E. and Rossi, A. P.: Characterization of geological settings related to intrusive magmatism on the Moon and Mars, Europlanet Science Congress 2024, Berlin, Germany, 8–13 Sep 2024, EPSC2024-466, https://doi.org/10.5194/epsc2024-466, 2024.
Abstract
We analyzed the structure of Atahensik Corona (700 x 900 km) of eastern Aphrodite Terra on Venus. This corona contains a high density of radial, oblique, and concentric fractures and is surrounded by arcuate troughs. The high density of concentric fractures along the outer rise indicates elastic down-bending of the corona´s surrounding. The deep, asymmetrical, and arc-shaped troughs are expressions of incipient subduction and expose large-scale fault zones along their steep inner slopes that trend parallel to the trough axes. The exposed faults are several hundred kilometers long and dip gently towards the corona center. The faults have a multi-stage history. They were initiated as thrusts but became reactivated as low-angle normal faults and then exposed parts of their fault surfaces. The multi-stage activation is in agreement with current models of corona formation. Plume uplift and topographic uplift of the corona interior are indicated by early radial fracturing. Subsequent lateral spreading of the plume steepened the outer rim and caused a fractured ridge annulus to form. Overthrusting in the corona periphery may have started in the immediate surrounding of a negatively buoyant, delaminated lithosphere, where the lithosphere was intact and cooler. Reactivation of the thrusts as low-angle normal faults resulted from subsidence of the corona´s interior as a consequence of decreased activity and cooling, and subsequent gravitational instability of the elevated corona annulus.
Introduction
Coronae are unique volcano-tectonic features on Venus that transport heat from the mantle to the surface. Large coronae are roughly circular to ovoid, contain a fractured ridge annulus, and are surrounded by arcuate troughs and outer rises [1-2]. The central regions of coronae may contain volcanic edifices [3]. The majority of geodynamic models of corona formation postulate a buoyant magma diapir that rises through the mantle [3-5] followed by a lateral spreading of the plume. Other models suggest that coronae result from Rayleigh–Taylor instability of the mantle [6] or by magmatic loading of the crust.
Fig.1 Magellan SAR image (left looking) of Atahensik Corona and NW-SE topographic profile across the structure.
Data and Methods
We used NASA´s Magellan synthetic aperture radar (SAR) global mosaics, which have a spatial resolution of ∼75 m per pixel in this region [7], and DEM that is based on a combination of Magellan global topography data records and a stereo imagery cross-correlation of SAR data [8]. For mapping of radar images using ArcGIS 10.7, we have adopted a black-and-white inversion approach for the SAR data. Measurements of strike and dip of faults were carried out with the LayerTools plugin for ArcGIS [9].
Results and Interpretation
Atahensik is one of the largest coronae on Venus (Fig.1). It has an asymmetric, eye-shaped form and comprises several asymmetric and arc-shaped troughs. The convex sides of the troughs are flanked by broad and gentle outer rises. The troughs have asymmetric topographic profiles (Fig.1) with a gentle outer slope and a steep inner slope that merge into the Atahensik´s annulus ridge. The central region of Atahensik Corona is morphologically depressed (Fig.1).
Fig.2 Fractures and major faults of Atahensik. The orientation of fractures relates to Atahensik´s center.
Atahensik Corona has a high density of fractures (Fig.2). A detailed analysis of crosscutting relationships between the fracture systems indicates that radial fractures in most cases developed first, followed by oblique, and finally concentric fractures. The inner slopes of the arcuate troughs show abrupt changes in SAR reflectivity (Fig.3) and major fault traces parallel to the trough axes were detected. Radial fractures do not continue from the convexly shaped hanging wall to the footwall of the faults. The faults strike concentrically and gently dip to the corona center. The smooth fault planes are partly exposed and form terraces in the slope profiles. This can only occur in a normal faulting regime when the hanging wall is displaced and exposes parts of the fault plane. The observation that the faults are low-angle normal faults is in contrast to the trough asymmetry, the presence of an outer rise, and the fracture pattern that all indicate lithospheric bending associated with overthrusting and incipient subduction (Fig.1). The apparent contradiction is resolved when a reactivation of the fault with the opposite shear sense is assumed. We propose that the faults were initially formed as thrusts during incipient subduction with a typical dip of ~30° towards the corona but were reactivated as a low-angle normal faults, thereby exposing their fault planes. A fault reactivation is expected when the horizontal compressive stresses radial to the corona, e.g. by down-welling decrease and the topographically high ridge annuli forming the rim of Atahensik Corona become gravitationally unstable in a phase of declining magmatic activity. The multi-stage activation agrees with the evolutionary sequence proposed for corona formation. Fault reactivation is a well-known phenomenon on Earth and low-angle normal faults are widely recognized [10]. The reactivation of a thrust fault as a low-angle normal fault requires a significantly reduced friction coefficient. On Earth, this is achieved by the presence of ductile shear zones, phyllosilicates, or a fluid overpressure. In the absence of hydrous phases and fluids on Venus, a decrease in fault strength and friction coefficient might be achieved by abrasive smear of rocks associated with thermally activated crystal plasticity or the lubrication of the fault plane by a melt film, possibly of a frictional origin.
Fig.3 Inverted SAR of the SE Atahensik trough with tectonic labels, LayerTool line, and the average dip angle and dip azimuth of the major fault.
References:
[1] Smrekar, S.E., Stofan, E.R., 1997, Science 277, 1289-1294. [2] Sabbeth, L. et al. 2024, EPSL, 633, 118568. [3] Squyres, S.W. et al., 1992, JGR 97, 13611–13634. [4] Gülcher, A.J. et al., 2020, Nature Geoscience, 13(8), 547-554. [5] Hoogenboom, T. & Houseman, G.A., 2006, Icarus, 180, 292-307. [6] Tucker, W.S. & Dombard, A.J., 2023, JGR, 128, e2023JE007971. [7] Pettengill, G.H., et al., 1991, Science, 252, 260-265. [8] Herrick, R.R. et al. 2012, EOS, 93, 125–126. [9] Kneissl, T., et al., 2010, LPSC, 41, #1640. [10] Wernicke, B., 1995, JGR 100, 20159-20174.
How to cite: Kenkmann, T. and Karagoz, O.: Low-angle faults at the rim of a large Venusian corona, Europlanet Science Congress 2024, Berlin, Germany, 8–13 Sep 2024, EPSC2024-383, https://doi.org/10.5194/epsc2024-383, 2024.
The surface of Venus presents a large variety of tectonic structures, from rift zones that extend thousands of kilometers [1], to globally spread wrinkle ridges [2] and coronae that could be associated with regional subduction [3]. In addition, there is a growing number of observations that point towards a geologically active Venus at present-day [4,5]. Therefore, it is highly likely that Venus is currently a seismically active planet. Yet, very little is known about the seismicity of Venus, mostly due to the lack of seismic data. Meanwhile, taking other geophysical constraints, we can start investigating some seismic properties of Venus. These analyses are essential for the planning of potential future seismic-focused missions to Venus.
A fundamental property to characterize possible seismicity levels of a planet is the thickness of the seismogenic zone, which corresponds to the upper, more brittle part of the planet where rocks can break and release seismic energy. The seismogenic thickness is closely related to the thermal structure of the lithosphere and it is usually defined by an isotherm. This study compiles estimates of lithospheric thermal gradients from geodynamic models and geophysical observations with the goal of obtaining a holistic view of the lithospheric thermal structure and seismogenic zone thickness of Venus. Here we adopt the 600°C isotherm as the seismogenic thickness, based on what has been measured for the Earth [6].
We use three independent approaches to investigate the thickness of the seismogenic zone on Venus. In the first approach, we compile a range of local elastic thickness constraints based on flexural analysis using topography and gravity data from different studies [7,8,9,10]. These elastic thickness estimates are then used to compute lithospheric thermal gradients which, in turn, allow us to determine locally the depth of the 600°C isotherm. Considering a strain rate of 1e-16 s-1 and a dry diabase rheology [11] we found that seismogenic thickness values range from 4 to 30 km, as shown in Figure 1a.
In a second approach we use 3D geodynamic thermal evolution models to assess the thermal structure of present-day lithosphere considering two distinct end-member magmatic scenarios [12]. In one case, we consider fully extrusive magmatism, i.e., all melt produced in the mantle is extracted to the surface. On the second case, 80% of the melt remains trapped within the lithosphere at 50 km depth. These scenarios lead to completely distinct lithospheric structure (see Figure 1b). Extrusive magmatism builds an extremly thick and cold lithosphere aassociated with seismogenic thicknesses of 60-150 km, while a high level of intrusions results in a thin and warm lithosphere, with seismogenic thickness values of 5-40 km.
Finally, we obtain seismogenic thickness estimates associated with constraints on mantle density anomalies from geophysical inversions using gravity and topography data [13]. In this case, the density anomalies are assumed to be caused by mantle temperature anomalies via the relation , where is the thermal expansivity, is the reference mantle density and correspond to latitude and longitude. These mantle temperature anomalies cause temperature variations at the base of the thermal lithosphere which, in turn, affect the lithospheric thermal gradient and the seismogenic thickness. Since these constraints are only sensitive to lateral variations of temperature and not the absolute temperature, to constrain the seismogenic thickness we use the intrusive geodynamic model as a reference temperature profile. Figure 1c shows the seismogenic thickness map, using K-1 and kg/m3. In this approach, the estimates range from about 15-45 km.
Figure 2 summarizes the results from the three different approaches, where the top plot presents the thermal gradient estimates, and the bottom plot shows the seismogenic thickness estimates. The left panels correspond to estimates from local flexural analysis for two different rheologies, the center panels show the geodynamic model estimates for the fully extrusive and 80% intrusive case, and the right panels are associated with the estimates from mantle density anomalies. For the latter, the two cases shown correspond to end-members parameters associated with maximum variability (density anomalies are modeled as a thin mass-sheet and K-1) and minimum variability (density anomalies assumed to be radially constant throughout the mantle and thermal expansivity of K-1) of seismogenic thickness estimates.
From the observational constraints and the highly intrusive model scenario we find that the seismogenic thickness of Venus ranges from about 4 to 40 km. The constraints from flexural analysis are related to the largest thermal gradient estimated (and thinnest seismogenic zones). This is likely because many of the investigated features are associated with locally anomalous temperatures, probably associated with magmatic processes [10]. It is also important to note that the thermal gradient estimates correspond to the time of formation of the features and it is possible that the thermal gradients are not as high at present day. Interestingly, the high intrusive geodynamic model also reaches high thermal gradient values (above 20 K/km) locally where there has been recent emplacement of intrusive melts (see Herrera et al., this meeting, for more details). Nevertheless, our results indicate that the background thermal gradient of Venus ranges from 5-10 K/km which is associated with seismogenic thicknesses of roughly 10-30 km.
References:
[1] Foster and Nimmo 1996, EPSL [2] Billoti and Suppe 1999, Icarus[3] Davaille et al. 2017, Nature Geoscience [4] Smrekar et al. 2010, Science [5] Herrick and Hensley 2023, Science [7] O’Rourke and Smrekar 2018, JGR: Planets [8] Borrelli et al. 2021, JGR: Planets [9] Maia and Wieczorek 2022, JGR: Planets [10] Smrekar et al. 2023, Nature Geoscience [11] Mackwell et al 1998, JGR [12] Plesa et al. 2023, EGU [13] Maia et al. 2023 GRL
How to cite: Maia, J., Plesa, A.-C., van Zelst, I., Brissaud, Q., De Toffoli, B., Garcia, R., Ghail, R., Gülcher, A., Horleston, A., Kawamura, T., Klaasen, S., Lefèvre, M., Lognonné, P., Näsholm, S. P., Panning, M., Smolinski, K., Solberg, C., and Stähler, S.: Constraining the Seismogenic Thickness of Venus, Europlanet Science Congress 2024, Berlin, Germany, 8–13 Sep 2024, EPSC2024-915, https://doi.org/10.5194/epsc2024-915, 2024.
The 2029 close Earth encounter of Near-Earth Asteroid 99942 Apophis presents a unique opportunity to study the dynamics, bulk properties, and interior structure of a potential rubble-pile asteroid [1]. Numerical models – including Finite Element Methods (FEM) and Discrete Element Methods (DEM) – are essential to constrain dynamical outcomes of the encounter and support planned and potential science missions to Apophis [2, 3].
The primary consensus from dynamical models of the encounter indicate that the most visible physical outcome of the close approach will be a change in the rotation state of Apophis [4, 5], and that Apophis will pass outside of the Earth’s Roche lobe and will thus not suffer a catastrophic disruption in this encounter if it is a rubble pile. DEM-only models [9, 10] point to a small or negligible and primarily elastic change of the body’s envelope.
Importantly, all of the dynamics, FEM, DEM, and combined models indicate that any physical changes to the structure or surface of Apophis as a result of the close encounter will be small [6, 7, 8, 9]. The small stress variations and elastic nature of the encounter open the door for a seismic study using DEM, where the individual particles act as seismic stations to track the propagation of waves through the body. Results from such models may be critical when determining the kinds of instruments or observations a mission should prioritize.
We present here an architecture for performing seismic investigations with DEM. We will also present new, preliminary soft-sphere DEM (SSDEM) results regarding the presence, timing and depth of seismic activity induced in Apophis during the close approach.
For the simulations presented here, we use the parallelized, N-body gravity and SSDEM tree code PKDGRAV to model gravitational and contact forces between discrete, spherical particles [10]. The SSDEM in PKDGRAV allows particles to slightly interpenetrate at the point of contact, using a Hooke’s law restoring spring force to model the material’s stiffness and apply damping and friction forces for particles in contact [11].
The most important parameters in modeling the propagation and attenuation of seismic waves in SSDEM are the choice of the spring constant in the normal direction (kn), and the damping parameters, respectively. The spring constant is akin to a Young’s modulus [10] and governs the wave speed in our models. We choose a kn equivalent to a Young’s modulus between 5-15 MPa (depending on particle radius) in our models, matching the values estimated by the Rosetta lander on comet 67P [12]. The energy-damping parameters influence wave attenuation and are chosen in conjunction with the frictional parameters to match our desired angle of repose for asteroid regolith: ~35 degrees [11].
We validate our seismic investigation method by modeling P-waves in simple 1-, 2-, and 3-dimensional structures: a particle chain, a grid, and a roughly spherical, densely packed rubble pile, respectively. We track the wave speed and attenuation in our models and compare them to the simulation input parameters mentioned above, to develop an interpretation from our discrete approach to the typical continuum-mechanics framework.
For the full Apophis encounter models, we follow the method of our previously published work, as described in [10]. Apophis is modeled as a 350-meter-diameter, cohesionless, self-gravitating granular aggregate of ~10,000 spherical particles, with shape matching the best-fit, radar-derived shape model [13], and Earth is a single sphere.
Each PKDGRAV particle can be used as a seismic station in our models, with velocities measured at every timestep (~0.038 s). We identify seismic sources inside the body from peaks in velocity profiles. Our preliminary analysis indicates that the quaking on Apophis will be shallow, with ~50% of sources occurring at a depth of ~30 m or less (see Fig. 1 bottom). Furthermore, our simulations show that most sources begin ~2 h after closest approach and persist for a period of ~2 h (Fig. 1 top). This period starting 2 h after close approach is the time when Earth’s gravitational influence on Apophis is becoming negligible compared to the local gravity and rotational forces and Apophis is settling into its new post-encounter equilibrium rotation state. Our results imply that it may be this change in rotational forces that induces seismicity in the near-subsurface of Apophis. These models also strongly support the inclusion of an in-situ seismic instrument [14] on any potential missions that will arrive at Apophis prior to its close approach in April 2029.
Acknowledgments: This work was supported in part by the Chateaubriand Fellowship Program, CNES, and by NASA FINESST Award 80NSSC21K1531. DEM simulations were carried out on the deepthought2 and Zaratan supercomputing clusters administered by the University of Maryland Division of Informational Technology.
References: [1] Binzel, R. et al. (2021) Planet. Sci. and Astrobio. Decadal Survey 2023-32, 53 (4) eid 045. [2] DellaGiustina, D. N. et al. (2023) Planet. Sci. Journal, 4 (10), 22 pgs. [3] Morelli, A. C. et al. (2023) arXiv 2309.00435. [4] Pravec, P. et al. (2014) Icarus 233, 48-60. [5] Benson, C. J. et al. (2023) Icarus 390, id 115324. [6] Kim, Y. et al. (2023) Mon. Not. Royal Astr. Soc. 520 (3), 3405-3415. [7] Yu, Y. et al. (2014) Icarus 242, 82-96. [8] DeMartini, J. V. et al. (2019) Icarus 328, 93-103. [9] Hirabayashi, M. et al. (2021) Icarus 365, id 114493. [10] Schwartz, S. R. et al (2012) Granular Matter 14, 363-380. [11] Zhang, Y. et al (2017) Icarus 294, 98-123. [12] Möhlmann, D et al. (2018) Icarus 303, 251-264. [13] Brozović, M. et al. (2018) Icarus 300, 115-128. [14] Murdoch, N. et al. (2024) EPSC
Figure 1. Top: Frequency of seismic events per hour. The region of significant tidal influence is bracketed by the green and red dashed lines. Time of closest approach is marked with a black dashed line. Bottom: Frequency of seismic events at varying depths, with bins ~15 m wide.
How to cite: DeMartini, J., Murdoch, N., Garcia, R., and Richardson, D.: SSDEM Discrete Seismology Models with Applications to the Apophis 2029 Close Earth Encounter, Europlanet Science Congress 2024, Berlin, Germany, 8–13 Sep 2024, EPSC2024-737, https://doi.org/10.5194/epsc2024-737, 2024.
A new development in the field of adaptive optics (AO) on ground-based telescopes enables routine monitoring of changes on Io's surface at scales down to ~80km (achieved), or even down to ~50km (in the limit). Our observations, taken with SHARK-VIS on the Large Binocular Telescope (LBT) in Arizona, demonstrate this new capability. SHARK-VIS adds a visible light science channel to the AO system at LBT. While AO science in the infrared has been widespread for decades, visible-light AO science is new. SHARK-VIS, which saw first light at LBT on October 2nd, 2023, is one of only a few visible-light AO instruments on large telescopes.
Our images of Io, taken soon after first light, are of the highest spatial resolution ever attained from a ground-based telescope. In addition to confirming known surface features, these images show a previously unseen plume deposit that obscures a portion of Pele's persistent red ring (see Fig. 1). This plume deposit, we believe, came as the result of a powerful eruption at Pillan Patera.
Figure 1. The SHARK-VIS detection image on Nov. 23, 2023 (upper left), and again on Jan. 10, 2024 (upper right), and the reprojection of the Voyager and Galileo spacecraft-derived Io photomomosaic for Jan. 10, 2024 (center) (Becker & Geissler, 2005).
To determine the date of the Pillan eruption, we analyzed thermal emission data collected by other telescopes over the last four years. Although these infrared images were necessarily taken at lower spatial resolution (due to the wavelengths used), the spatial resolution is sufficient to detect if and when excess thermal emission might have originated from Pillan Patera. These data show a spike in thermal emission, indicating a powerful eruption, during August 2021. Augmented with data from the Juno JIRAM instrument, we believe that this spike corresponds to the eruption responsible for the plume deposit seen in the SHARK-VIS images.
These SHARK-VIS images serve as a demonstration of how adaptive optics at visible wavelengths will allow us to monitor surface changes on Io at regular intervals. Note that, prior to the SHARK-VIS observation, the most recent high-resolution imaging of the Pele region was from the New Horizons fly-by during March 2007. By April 2024, as seen by the visible imager on the Juno spacecraft, the red ring around Pele had repaired itself. Without the SHARK-VIS images, this resurfacing event would have never been detected.
To date, regular monitoring of Io using ground-based facilities has largely been restricted to M-band (4.8 μm) imaging which, even using adaptive optics on 8-10 metre telescopes, yields spatial resolution of about 400-600 km. While there will always be a need for infrared images of Io for the thermal data that informs volcanology, visible-light images at 50-80km resolution allow us to "see" the landscape, to more accurately locate the effects of eruptions and associated features such as plume deposits.
In our presentation, we will provide details of the Pillan plume deposit and its encroachment onto Pele's ring, and how that observation serves as a demonstration of how we will be able to monitor surface changes on Io going forward. We will also describe future ground-based systems that could produce imaging of Io down to spatial scales below 12km.
How to cite: Conrad, A., Pedichini, F., Li Causi, G., Antoniucci, S., de Pater, I., Davies, A. G., de Kleer, K., Piazzesi, R., Testa, V., Vaccari, P., Vicinanza, M., Power, J., Ertel, S., Shields, J. C., Ragland, S., and Giorgi, F.: Pele meets Pillan: Demonstration of a new method for monitoring surface changes on Io, Europlanet Science Congress 2024, Berlin, Germany, 8–13 Sep 2024, EPSC2024-147, https://doi.org/10.5194/epsc2024-147, 2024.
ABSTRACT
Previous studies have suggested that extrusive magmatism efficiently cools planetary interiors but the contribution by intrusive magmatism has been little investigated so far. We study the effects of the magmatic style (i.e., intrusive vs. extrusive magmatism) on the thermal evolution of Mercury-, Venus-, Moon-, and Mars-like bodies. Our results suggest that different magmatic styles strongly affect the thermal evolution of planets, where for instance intrusive magmatism allows for thinner lids, cooler melts and more melt production. In addition, for large and/or highly magmatically active planets such as Venus, an intrusive magmatism allows for more efficient cooling of the interior.
INTRODUCTION
Volcanic activity has been evidenced on planetary bodies across the inner solar system [1]. Mercury's volcanic surface expressions are extrusive volcanic vents, pyroclastic deposits, lava flow margins, etc.; and studies have analyzed their history in terms of the effect of the planetary cooling who led to the global contraction [2,3]. Venus surface is dominated by volcanoes, flow fields, volcanic vents, and coronae, among other features [4]. Recent analysis of radar data collected by the Magellan mission suggests that there could be volcanic activity still ongoing on Venus [5].
Volcanism has also shaped the lunar surface, leading to the formation of a variety of volcanic landforms such as lunar maria, lava flows, domes, cones, etc., features that were confirmed after a series of lunar exploration missions and even directly studied thanks to the return of samples from the lunar surface [6,7]. The extensive volcanic products on Mars account a large variety of explosive [8] and sedimentary volcanism [9], and recent studies presented geophysical evidence for active volcanic processes in the Elysium Planitia region [10,11].
These volcanic features are witnesses of magmatic processes that these bodies have experienced, but the amount of intrusive vs. extrusive melt that was produced during the thermal history is difficult to constrain. Extrusive magmatism has been suggested to allow more efficiently cooling of planetary interiors, but the role of intrusive magmatism on the thermal evolution has been little investigated.
In this study, we analyze the effect of the magmatic style (i.e. ‘fully intrusive’ vs. ‘fully extrusive’ magmatism end-members) by modelling the thermal evolution of Mercury, Venus, Moon, and Mars-like bodies. Our aim is to understand the effect of different magmatic styles for different planetary interiors rather than the particular evolution of the inner solar system bodies.
METHODS
We use the mantle convection code GAIA in a 2D spherical annulus geometry [12, 13]. Our models employ a temperature- and pressure-dependent viscosity that follows an Arrhenius law for diffusion creep [14, 15]. The strong temperature-dependence of the viscosity leads to the formation of a stagnant lid (an immobile layer) at the top of the convecting mantle, due to the cold temperature conditions. The thermal conductivity and thermal expansivity in our models are pressure- and temperature-dependent and we use parametrizations derived from ab-initio calculations and laboratory experiments [16]. We assume a homogeneous distribution of the heat sources and account for the decay in time of radioactive elements (i.e. 238U, 235U, 232Th, and 40K) and consider that the core cools with time.
Melting occurs when the mantle temperature exceeds the melting temperature. To keep the models as best as possible comparable with each other, we use the same melting curve parametrization as derived for the Earth’s interior [17]. We compute partial melting and consider two scenarios, i.e., fully intrusive and fully extrusive magmatism (Fig. 1). For all bodies, the depth of magmatic intrusions is set at 50 km depth. For scenarios where partial melting occurs deeper than the density crossover at ~11GPa [18], the melt is not buoyant enough to rise towards the surface and it is thus not considered in our models.
RESULTS
For all studied bodies, the convection pattern is characterized by stronger mantle plumes and more vigorous mantle flow for the fully intrusive cases than for the fully extrusive cases (Fig. 2). Additionally, the intrusive melt depth seems to control the stagnant lid growth with thinner lids for cases with magmatic intrusions.
While the global average temperature of the entire silicate part is higher for Mercury, Mars, and the Moon in the intrusive scenario compared to extrusive models, for Venus the opposite is the case (Fig. 3a). We explain this by Venus’s smaller lid-to-mantle thickness ratio and high melt production rate compared to Mercury, Mars, and the Moon. Normalized to their silicate mantles, the intrusive magmatism models produce more melt than the extrusive cases (Fig. 3d).
The mechanical lid depth of the intrusive cases is always shallower through time (Fig. 3b), diverging from the extrusive cases up to hundreds of kilometers. This is explained by higher thermal gradients and thus warmer lithospheres in the intrusive cases.
Mercury cools very quickly compared to the other planets and stops producing melt after the first half of its evolution (Fig. 3c). After that moment, the differences between the two scenarios are nearly identical. For all bodies, the intrusive magmatism cases melt at shallower depths with cooler melts during their evolution.
SUMMARY
Throughout the evolution of all studied bodies, the fully intrusive cases present thinner mechanical lids, cooler melt temperatures, more melt production, and shallower melting depths than the extrusive cases. Our results suggest that large and/or highly magmatically active planets such as Venus efficiently cool their interior through intrusive magmatism, while keeping at the same time a warm and thin lithosphere.
REFERENCES
[1] Byrne et al., Nat.Astron, 2020; [2] Thomas & Rothery, Elements, 2019; [3] Wright et al., J. Volcanol., 2021; [4] Ghail et al., Space Science Reviews, 2024; [5] Herrick & Hensley, Science, 2023; [6] Head, Rev Geophys., 1976; [7] Zhao et al, Space: Science & Technology, 2023; [8] Brož et al., J. Volcano., 2021; [9] Brož et al., Earth Surf. Dynam., 2023; [10] Broquet & Andrews-Hanna, Nat.Astron., 2023; [11] Stähler et al. Nat.Astron., 2022, [12] Hüttig et al., PEPI, 2013; [13] Fleury et al., Geochem.Geophys., 2024; [14] Karato et al., JGR, 1986; [15] Karato & Wu, 1993; [16] Tosi et al., PEPI, 2013; [17] Stixrude et al., EPSL, 2009; [18] Ohtani et al., Chem. Geol., 1995.
How to cite: Herrera, C., Plesa, A.-C., Maia, J., and Breuer, D.: Effects of magmatic styles on the thermal evolution of planetary interiors, Europlanet Science Congress 2024, Berlin, Germany, 8–13 Sep 2024, EPSC2024-650, https://doi.org/10.5194/epsc2024-650, 2024.
Wrinkle ridges (WRs) are among the most prevalent tectonic landforms observed on terrestrial planetary bodies. They are characterized by highly variable, positive relief, which exhibit linear, sinuous, and discontinuous morphologies, sometimes bifurcating or forming en-echelon arrays. They are interpreted as folds overlying blind thrusts, which can reach reliefs of 100’s meters and widths of several 10’s kilometers.
On Mars, WRs typically occur on flood basalt-like units on volcanic plains and within large impact basins. Their analysis can yield valuable insights into the geological evolution of Mars. The structural style of WRs can be used to infer lithospheric strain accommodation, also giving insights onto the mechanical properties of the involved crust.
WRs formation remains a topic of debate with unresolved questions, including: i) geometry and likely structural style of associated blind faults, ii) fault depth, iii) number and role of faults, iv) amount of shortening. Various methodologies have been employed to address these questions, such as elastic dislocation modeling, boundary element modeling, and balancing techniques [1 for a review]. However, these approaches do not completely describe the entire spectrum of observations related to WRs morphometry and kinematics.
In this work, we use the Move software (Petex) to conduct a 3D geometrical reconstruction of a set of WRs, by analyzing and reproducing their morphometric characteristics. We perform a detailed kinematic analysis on nine WRs: six in the circum-Tharsis regions of Lunae Planum and Solis Planum, while further three in Hellas Planitia, Hesperia Planum and Syrtis Major Planum (Fig.1), which underwent different tectonic evolutions.
Fig.1. (a) Map view of the study areas (white squares) and insets (b, e, l) for Symmetric, (c, f, i) for Asymmetric and (d, g, h) for Double ridges WRs.
Adhering to the most recent WR classification proposed by [2], we choose representative examples of each WR type, including symmetric, asymmetric, and double. We prioritize homogeneous topographic data resolution, primarily derived from the Mars Orbiter Laser Altimeter (MOLA). The erosion rates on Mars are constrained between 0.01 to 10 nm/yr [3]. Therefore, by considering areas unaltered by e.g., channels, impact craters, landslides, the topography can be considered as a direct product of deformation.
We apply the Trishear and Fault-Parallel-Flow integrated forward kinematic modelling to model WRs related faults. Trishear allows deformation in the fore-limb of a fault propagation fold, which is confined in a triangular zone radiating from the fault tip, characterized by non-uniform deformation. Within the triangle zone, layer thickness and length can change during deformation, but the area is kept constant [4]. Fault-Parallel-Flow algorithm is a scale-independent method describing how hanging-wall rocks are displaced parallel to the complex fault plane. The methodology allows to model complex fault geometries by assuming area conservation and plane-strain deformation, to determine the fault geometry and kinematics that best fits the observed topography and the measured outcropping faults dip angles.
Our results demonstrate the reliability of the trishear method to model planetary WRs and provide an improvement in understanding Mars’ lithospheric mechanical stratigraphy and WRs kinematics. We demonstrate how the wrinkly and complex nature of WRs can be related to the presence of multiple faults, which accommodate shortening differently (Fig.2).
Fig. 2. 3D model at Lunae Planum (a) and Solis Planum (c). Best-fitting results as true Z difference between modelled and original topography (b, d).
Along the studied asymmetric WRs, the master faults accommodate ca. 60–100% of the total modelled slip, depending on the presence of backthrusts. Along the studied double ridge WRs, characterized by a master fault and a series of smaller backthrusts, the master faults accommodate ca. 40–60% of the total modelled slip. On the symmetric WRs, characterized by a master fault and a main backthrust, the symmetry is given by the master fault and its closest backthrust, whose slip is higher. The master fault and backthrust accrue the 32–54% and the 37–68% of the total modelled slip, respectively. We also model a series of synthetic thrust faults, which promote a further shortening partitioning. Such outcomes may be indicative of an heterogenous mechanical stratigraphy, characterized by multiple shallow detachments, suggested to be likely found within sedimentary interlayers.
The results of the trishear kinematic modelling indicate correlations of the main morphometric parameters of WRs with the geometry and kinematics of the faults (Fig.3).
Fig. 3. (a) Relief (H) vs. slip (S): crest relief (HC) against slip of faults below the ridge (SC), and ridge relief (HR) against slip of all faults (Stot); (b) elevation of fault upper tips (ZTop) against crest width (WC); (c) spacing of the faults below the ridge (LCF) against crest width (WC); (d) ridge crest location (LRC) against location of fault dip change at depth (LT).
The correlations are based on the Ordinary Least Squares Linear Regression, whose quality is represented by the Coefficient of Determination (R2), integrated with residual plots. The good fitting between the parameters can help in a fast correlation between the main morphometric characteristics of WRs with both the geometry and kinematics of the faults at depth. WRs characterized by a higher relief are driven by larger amounts of horizontal along-fault slip, while the broader the width of the main crest, the deeper and more spaced are the faults below the crest (i.e., master fault and possible backthrust). The location of the hinge zone of the main crest, corresponds to the fault dip change at depth. However, the specific depth at which the dip change occurs is not correlated and mainly depends on the dip angle of the upper fault tip, which may vary case by case.
[1] Karagoz, O. et al. (2022). Icarus, 374, 114808. [2] Andrews-Hanna, J.C. (2020). Icarus, 351, 113937. [3] Golombek, M.P. et al. (2006). JGR, 111 (E12S10). [4] Pei, Y. et al. (2014). JSG, 66, 284–297.
How to cite: Carboni, F., Karagoz, O., and Kenkmann, T.: Trishear Forward Modelling of WRs on Mars: morphometry and kinematics correlation to unravel Mars geology, Europlanet Science Congress 2024, Berlin, Germany, 8–13 Sep 2024, EPSC2024-888, https://doi.org/10.5194/epsc2024-888, 2024.
Introduction
Mercury’s Discovery quadrangle is located at southern mid-latitudes in a heavily cratered region roughly antipodal to Caloris Basin [1]. The quadrangle hosts a probable pre-Tolstojan multi-ring impact basin named Andal-Coleridge, surrounded by a three- to five-ring system [2,3].
Here we present a high-resolution structural map of the quadrangle that will contribute to the 1:3M quadrangle geological map series in preparation for the BepiColombo mission [4]. In addition, we carried out a structural analysis in order to study the structural framework of the quadrangle, validate and ascertain the existence of the Andal-Coleridge basin and investigate its influence on the tectonic evolution of this region.
Data and methods
We produced a high-resolution structural map of the quadrangle utilizing MESSENGER end-of-mission products [5]. Structure strikes were then plotted in rose diagrams to recognize preferential trends at the regional scale. We also investigated the structural relationships between three main scarps (Discovery, Adventure and Resolution Rupes – DAR) –including another scarp (here named Discovery-2) that seems to be the westward continuation of the Discovery Rupes (Discovery-1)– by making several profiles across them and measuring their throw. Furthermore, to validate and ascertain the presence of the Andal–Coleridge basin, we employed gravimetric data and estimated the related stress field via beta-analysis.
Map and trend of structural features
Our structural map (Fig.1) reveals ∼500 segments of contractional structures –including lobate scarps, high-relief ridges and wrinkle ridges– mainly arranged in a circular pattern at the approximate centre of the quadrangle, encircling both a broad topographic low and a mascon, similar to Caloris Basin [6], although identified only in the Bouguer anomaly map of [7]. Strike directions of the segments within rose diagrams generally show a uniform distribution of bins –together with a NW-SE preferential trend– suggesting an impact-related nature for most structures [8].
Figure 1 Structural map of the Discovery quadrangle overlayed to the Digital Elevation Model of [9] (left) and the Bouguer Anomaly Map of [7] (right). The red dashed line approximately delimits the topographic low and the mascon respectively.
Beta-Analysis
Following the work done for Mercury and Mars by [2] and [10], we estimated the stress field related to concentric structures via beta-analysis. This approach reveals a bimodal distribution consisting of a primary "bull's-eye" distribution, whose centre represents the point from which the causative stress field for faults spread, and a secondary, much less dense, distribution (Fig.2). Discovery Rupes aligns concentrically with the primary distribution, while Adventure and Resolution Rupes exhibits concentric alignment with the secondary distribution roughly coincident with another probable impact basin, informally named b78 [11], where another smaller mascon is present.
Figure 2 (left) The stress field resulting from beta-analysis in stereographic projection centred at quadrangle’s centre. (right) The hypothesised location and extent of Andal-Coleridge and b78 basins from [11].
Throw-Height Analysis
For each profile the scarp height was measured and then plotted against its position on the fault trace, corresponding to the fault length, resulting in a throw profile (Fig.3). The analysis of the throw profiles provide evidence that the three structures represent the morphological expression of two different faults, the Discovery fault and the Adventure-Resolution fault [2], grown hard-linking several segments together. These two faults also appear to be kinematically soft-linked, since the cumulative throw falls approximately at the centre of the system, consistent with terrestrial fault growth patterns [12]. Additionally, Discovery Rupes shows evidence of reactivation within Rameau crater, suggesting a process of fault-trace erosion and its subsequent re-emergence possibly due to Mercury's global contraction. Adopting previous dating of Rameau crater and Discovery Rupes [14,15], we derived a preliminary chronology for Discovery Rupes evolution and found a peak in throw-rate during the Tolstojan period, with declining activity towards the Mansurian period which is possibly continuing to the present [15].
Figure 3 (up) The DAR system and the 40 profiles used to produce the throw-height plot (down). Each peak on the plot represents a fault segment.
Conclusions and future work
The present work reveals a complex structural framework within Mercury’s Discovery quadrangle. The concentric alignment of structures to both a topographic low and a mascon together with the general uniform distribution shown in rose diagrams strongly supports the existence of the Andal-Coleridge basin. The concentricity of Discovery Rupes to the primary distribution identified through beta-analysis emphasizes its connection to the basin. In contrast, Adventure and Resolution Rupes display concentric alignment with the smaller b78 impact basin. This observation implies that these two scarps originated from two distinct impacts and were reactivated by Mercury's global contraction as a linked fault system. The Andal-Coleridge basin likely introduced mechanical discontinuities in the crust, influencing the localization and orientation of faults [2]. These weaker zones were eventually exploited during the subsequent global contraction. Indeed, the throw-height analysis shows signs of reactivation where Discovery Rupes cuts Rameau crater, suggesting a peak in throw-rate during the Tolstojan period.
We aim at improving the structural map of the quadrangle to better understand the NW-SE-trending structures’ behaviour and better investigate the fault reactivation. This study may also represent a contribution for evaluating the rate of global contraction and its magnitude throughout Mercury’s evolution.
Acknowledgements
We gratefully acknowledge funding from the Italian Space Agency (ASI) under ASI-INAF agreement 2017-47-H1.
References
[1] Trask and Dzurisin (1984). USGS, IMAP 1658. [2] Watters et al. (2001). Plan. and Sp. Sci., 49(14-15), 1523-1530. [3] Spudis and Strobell (1984). LPSC, 814-815. [4] Galluzzi et al. (2019). JGR: Planets, 124(10), 2543-2562. [5] Denevi et al. (2017). Sp. Sci. Rev., 214(1). [6] Smith et al. (2012). Science, 336. [7] Buoninfante et al. (2023). Sci. Rep., 13, 19854. [8] Delbo et al. (2019). LPI Contrib. No. 2189. [9] Becker et al. (2016). LPSC Contrib. No. 1903. [10] Wise et al. (1979). Icarus, 38, 456-472. [11] Orgel et al. (2020). JGR: Planets, 125(8). [12] Kim and Sanderson (2005). Earth-Sci. Rev., 68(3-4), 317-334. [13] Kinczyk et al. (2020). Icarus, 341, 113637. [14] Clark et al. (2024). LPSC Contrib. No. 3040. [15] Tosi et al. (2013). JGR: Planets, 118(12), 2474-2487.
How to cite: Sepe, A., Ferranti, L., Galluzzi, V., Schmidt, G. W., Buoninfante, S., and Palumbo, P.: Tectonic influence of multi-ring basins: The case of Mercury’s Discovery Quadrangle and the Andal-Coleridge basin., Europlanet Science Congress 2024, Berlin, Germany, 8–13 Sep 2024, EPSC2024-1106, https://doi.org/10.5194/epsc2024-1106, 2024.