Analogue missions serve as valuable models for simulating and testing scenarios for human space exploration in a terrestrial environment. The success of these missions relies on the seamless collaboration of diverse teams, each playing a crucial role in different phases of the mission lifecycle.  Among those teams the Remote Science Support (RSS) group, stationed at the Mission Support Center (MSC), stands out as an anchor connecting experts, scientists, and mission control center with analogue astronauts in the field.

The RSS plays a pivotal role in supporting Principal Investigators (PIs) throughout the entirety of the pre-mission, in-mission, and post-mission phases. During the pre-mission phase, the RSS team collaborates closely with PIs to fine-tune experiment parameters, ensuring their alignment with mission objectives and the unique challenges posed by analogue environments. The RSS team serves as a critical liaison, facilitating seamless integration of experiments into the analogue mission framework. In the synchronous (syn) mission phase, RSS operates in near real-time, providing immediate guidance and insights to astronauts as they execute experiments. This dynamic support ensures the optimization of decision-making processes and the resolution of mission-critical issues. Transitioning to the post-mission phase, RSS continues its support by facilitating data validation and scientific post-processing. By offering valuable insights and analysis, RSS assists PIs in refining future experiments and advancing their research agendas. This comprehensive support across pre, syn, and post-mission phases underscores the integral role of RSS in maximizing the scientific yield and success of analogue missions.

Communication delays, technological constraints, and the need for adaptable protocols present challenges for RSS. Recognizing the importance of these challenges, this study identifies strategies for mitigating them, emphasizing the need for interdisciplinary collaboration. Effective communication between the RSS team, Mission Support Center, and on-field astronauts becomes significant for overcoming these challenges. Continuous refinement of mission operations procedures is essential to ensure that the RSS remains a dynamic and responsive support system throughout the mission lifecycle.

The findings presented, contribute to the growing body of knowledge on analogue missions and underline the fundamental role of RSS in advancing human space exploration capabilities. As space agencies and research institutions continue to invest in analogue missions as a precursor to actual space expeditions, optimizing RSS mechanisms becomes paramount for achieving mission success and ensuring the safety and productivity of future astronauts.

How to cite: Knie, J., Özdemir-Fritz, S. Ö.-F., and Savic, J.: Mission operations – enhancing the success of analogue missions through the Remote Science Support (RSS), EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-22083, https://doi.org/10.5194/egusphere-egu24-22083, 2024.

In both real and analog missions, the crew can only perform activities and experiments outside the habitat for a certain amount of time. This means that the missions and therefore also the planned activities must be planned precisely to perform as many activities and experiments as possible in as short a time as possible. Such planning must consider external factors such as environmental factors, such as temperature or weather conditions, as well as the duration of experiments and dependencies on other experiments or activities. Furthermore, changes can occur continuously during a mission, which can also impact the planned schedule. In previous analog missions, this planning was performed manually, which can be very time-consuming due to the many possible conditions. This paper presents the Exploration Cascade, a mathematical algorithm that considers possible factors to create an optimal mission plan. Using the analog Mars mission AMADEE-24 as an example, we examine what results this algorithm can achieve and how flexibly it can react to changes, such as changes in weather forecasts or unforeseeable events, such as the failure of scientific equipment. Furthermore, we examined how the efficiency of the algorithm compares with manual planning and what conclusions can be drawn from it.

How to cite: Greif, F., Savic, J., Özdemir-Fritz, S., Grömer, G., and Lex, K.: The Exploration Cascade as a Mission Planning Algorithm for AMADEE-24, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-6855, https://doi.org/10.5194/egusphere-egu24-6855, 2024.

During the AMADEE24 mission in Armenia, the GEOS experiment focuses on geologic survey activities at the simulated Martian landing site.  GEOS applies classic geological field survey methods to a simulated mission to Mars, drawing on the experience of the lunar field survey built by Apollo missions.

The elements of GEOS are the mapping, the sampling, and the compositional measurements.  

The mapping phase involves developing mission-specific cartography from orbital remote sensing to large-scale mapping produced during and after the mission.  

The core element of GEOS is the sampling, providing the ground truth of the remote sensing observation.  AMADEE24 Rovers and Analog astronauts will do rock and terrain sampling along transects on base maps supplied by RSS (Remote Science Support) and Flight Planning (FP) for the Extra Vehicular Activities (EVAs).  Part of the samples will return from the simulated Martian habitat, and be made available for more advanced laboratory analyses.     

In-habitat compositional measurements offer a first estimate of the mineralogy and geochemistry of the samples.  Specifically, AMADEE24 carried a RAMAN spectrometer in the field.

 Here, we will present the preliminary results of AMADEE24/GEOS and ongoing activities for the technical and scientific exploitation of the experiment.

How to cite: Özdemir-Fritz, S., Frigeri, A., Schlinder, S., Willcocks, F., and Groemer, G.: The GEOS experiment onboard AMADEE24 crewed simulated mission to Mars, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-19916, https://doi.org/10.5194/egusphere-egu24-19916, 2024.

Analog research has become a common tool to devise scientific workflows and conducting technology developments for future planetary missions. In the past decade, a number of new analog facilities have emerge with a wide range of professionalism. Globally, more than a dozen active habitats are active, with a dozen missions annually each, with typically six to eight crew members. These are complemented with astronaut training field trips like the ESA PANGEA or CAVES initiative, or the NASA NEEMO missions.

The scientific quality and safety standards vary, as reflected in scientific productivity and safety track record. In recent initiative, a new industry standard is evolving measuring performance and risk management dubbed the “International Guidelines and Standards in Analogs” (IGSA), that strives to establish common sets of metrics to help devise a robust science program, management and safety standards as well as checklists to raise awareness for quality in analog research.

Such a guideline shall also help decision makers, mission managers and funding agencies aware of strength and weaknesses of analog campaigns. The first standard was approved for released in 2023 (IGSA-STD-1) by an international group of experienced analog mission managers and habitat directors, to a) improve space analog mission operations and safety, b) Create a more cohesive process across the space analog industry, c) Develop trust and integrity with the public, companies, nonprofit organizations, academia, researchers, innovators and funding agencies and d) develop a common language to measure and evaluate performance.

Applicable to habitat owners, individuals, crews, researchers, innovators and mission organizers wanting to participate in or conduct an analog mission, the IGSA-STD-2 has the objectives to a) protect mission organizers, directors, and analog astronauts by ensuring safety and quality control, b) allow interoperability of research and missions among habitats, c) Promote international collaboration, d) improve fidelity of research, e) improve synergy, eliminate duplication of effort, and optimize resources and other.

How to cite: Groemer, G.: The IGSA-STD-1 Standard: Measuring Mars analog missions quality, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-21635, https://doi.org/10.5194/egusphere-egu24-21635, 2024.

We develop a new crustal magnetic field model of Mars with spherical harmonic degree up to 140, which is based on orbiting measurements from Mars Global Surveyor (MGS), Mars Atmosphere and Volatile Evolution (MAVEN), and surface measurements from InSight and Zhurong. We follow the techniques from M14 model[Morschhauser et al., 2014] to inverse the spherical harmonic coefficients, including assigning different weights to the data of different sources, eliminating outliers with huber norm fitting, and employing the horizontal gradient of B_z component as L1 regularization term in the final model. It is found that our new model achieves the best spatial resolution ever before (~150 km). The unweighted misfits between our model and the MGS MPO, MGS AB/SPO and MAVEN are 8.0 nT, 9.9 nT, and 8.1 nT, respectively. Compared with the previous models, our model predictions are consistent with the surface measurements at InSight and Zhurong landing sites since the surface data are involved in the model inversion, which indicates the surface measurements are crucial to constrain the model downward continuation. The model characterizes the small-scale stratigraphic units on Mars, for example, the Lucus Planum, Apollinaris Patera, Hadriaca Patera, etc., contributing to the research of the structures of magnetic anomalies on Mars with different scales and the evolution of Martian dynamo.

How to cite: Tian, L. and Luo, H.: A crustal magnetic field model of Mars with spherical harmonic degree up to 140, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-2458, https://doi.org/10.5194/egusphere-egu24-2458, 2024.

Martian tectonic structures such as wrinkle ridges and lobate scarps exhibit differences in fault morphology and spacing across the Martian crustal dichotomy. On Earth, inherited structures from ancient tectonic activity may act as primary control in intraplate deformation. This hypothesis is yet to be explored for intraplate settings on other terrestrial planets, such as Mars. Large impact events during the Late Heavy Bombardment may have deeply fractured the Martian crust and mantle-lithosphere creating weakened inherited structures. Here, we hypothesize that Martian fault morphology may be controlled by subsurface deep impact cratering, and test using lithospheric-scale numerical models.

In this study, we use the open-source geodynamic code ASPECT (Advanced Solver for Planetary Evolution, Convection, and Tectonics) to investigate the role of impact-related inherited structures on intraplate fault morphology in different lithospheric settings. We present a suite of 2-D numerical lithospheric models under horizontal shortening comparable to that of global contraction. Model parameters are constrained by past Martian modelling efforts and seismic data from the recent InSight mission. However, given the uncertainty in thermal and rheological model parameters for the Martian lithosphere, we extensively test appropriate ranges to analyze their potential role and focus on the lithospheric thickness across the Martian dichotomy. Our modelling results show appropriate faulting at the surface that may be related to Martian wrinkle ridge and lobate scarp morphology and also offer potential subsurface scenarios of deep lithosphere fault networks on Mars. Similar to Earth tectonics, we indicate that deep lithospheric inheritance may provide control over surface fault morphology and spacing, providing new insight into the growth of intraplate faults across the Martian crustal dichotomy.

How to cite: Rich, J., Heron, P., and Crane, K.: The influence of deep impact cratering on Martian intraplate faults, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-12645, https://doi.org/10.5194/egusphere-egu24-12645, 2024.

The ARTEMIS program was launched by NASA to send astronauts back to the Moon to establish a permanent presence. The ARTEMIS missions will pave the way for the next big step—the launch of the first humans to Mars—by utilizing the Moon.

Unlike the Apollo missions, ARTEMIS missions are targeting the Lunar South Pole because of the Points of Interest such as the presence of water ice in the Permanently Shadowed Regions (PSR) in the craters, Peaks of Eternal Light (PEL) with high solar illumination, and constant contact with Earth.  On the lunar surface, a crew can travel two kilometres on foot, ten kilometres in an unpressurised rover, and twelve kilometres in a pressurised rover from the Human Landing System (HLS). Security reasons dictate these distances, enabling the crew to return to the HLS in an emergency. There is a clear gap between the points of interest and the safe landing spots identified in the frame of the ARTEMIS program.

A Secondary Habitat such as EUROHAB will close the gap between the safe landing spots and the points of interest. EUROHAB is an inflatable, deployable habitat delivered as a payload on a medium-size robotic lander (such as the ESA Argonaut/EL3 or the NYX of The Exploration Company) to the surface of the Moon. If placed strategically on the Lunar surface, EUROHAB not only will act as an outpost or a base camp to extend the range of exploration but also as a safe haven in case of off-nominal scenarios where the crew can take refuge. Additionally, EUROHAB can also serve as a teleoperated science station with experiments running autonomously, a storage place that can be utilized by the next missions, and assist Lunar surface assets like a rover for lunar night survival. 

A full-scale prototype was developed based on a CNES study (named “LISE”) to develop a lunar habitat that can be brought to the Lunar surface by ESA's Argonaut Lander to serve as a secondary habitat for the Artemis missions. EUROHAB II scale one prototype was exhibited at Assemble Nationale, Paris in June 2023. This platform will serve to test subsystems like the Life Support System, Energy Management, Robotics or Communication. EUROHAB could be a French or European contribution to Artemis which also makes use of other ESA elements of lunar logistics like the communication and navigation network MOONLIGHT.

EUROHAB II will be setup in Tignes, France for a five-day simulation mission from 22nd January 2024 to 26th January 2024 to test several aspects related to the mission simulation and system testing. The objective of this mission is to test the system in a harsher analogue environment (high altitude and polar conditions). Also, the team expects to test different internal configurations of such Secondary Habitat. The paper will detail the results of the analogue simulation activity.

How to cite: Singh, N., Weiss, P., Pouget, T., and Makthoum, M.: EUROHAB II: A Lunar Secondary Habitat platform for Space Analogue Mission, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-12403, https://doi.org/10.5194/egusphere-egu24-12403, 2024.

Although mechanisms of impact cratering have been studied intensely by numerical modelling and field analyses, an outstanding problem concerns long-term crater modification. Localized deformation in form of radial and concentric crater floor fractures are prominent post-cratering structural vestiges of lunar impact craters. Two mechanisms were proposed to explain the formation of floor fractures: isostatic re-equilibration of crust underlying crater floors, and emplacement of horizontal igneous sheets below craters. Due to thick and cool lunar upper crust, the latter mechanism has been regarded as the more plausible one to account for the presence of floor fractures in lunar craters. However, the structural consequences of magmatic inflation on surface deformation in combination with crater floor morphology has not been analyzed systematically in 3D.

We use scaled analogue experiments to model the deformational behavior of upper crust following crater formation to explore the structural and kinematic consequences of sill formation below crater floors with different depths and diameters. Our experiments were scaled to the lunar physical conditions. The initial diameter-to-depth ratios of lunar craters were based on numerical modelling. Granular material simulating the Moon’s brittle upper crust was filled into a 60 cm by 60 cm size tank. Craters with specified morphologies, depths and radii were “drilled” into this material by a rotating blade. Sills were simulated by variably sized flat, circular balloons of plastic foil, emplaced into the granular material below model craters and inflated by a pumped-in fluid. For each experiment, the sill was first inflated and then deflated to model intrusion and evacuation of magma, respectively. Surface deformation within and around the crater was monitored with a 4-D digital image correlation system allowing us to quantify key parameters including surface uplift as well as the distribution and evolution of strain. The results of our scale models enabled us to quantify the geometry and distribution of brittle deformation of lunar upper crust.

Our experiments show that inflation of balloons caused radial and concentric dilation fractures in the overlying granular material. Fracture patterns were more controlled by the depth to the top surface of balloons rather than by crater floor morphology. For the duration of fluid inflation into shallow model sills, surface uplift was focused in the crater center and associated with rather prominent fractures. Upon deflation, concentric normal faults developed at the inner crater rim, and this corresponds to the terraced crater margins ubiquitously observed at lunar craters. Interestingly, model craters are characterized by more diverse fracture patterns, compared to lunar craters. This may be due to brittle deformation above sills during inflation, allowing for magma to erupt from natural sill reservoirs. It is, therefore, unlikely that natural sill systems attain the structural maturity of our modelled equivalents. Hence, evacuation during inflation in natural systems can account for the presence of less prominent fracture patterns compared to the ones in modelled, more “mature” sill systems.

How to cite: Eisermann, J. O. and Riller, U.: Structural consequences of sill formation below lunar craters inferred from scaled analogue experiments, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-1299, https://doi.org/10.5194/egusphere-egu24-1299, 2024.

Throughout the Solar System, large infilled basins exhibit a variety of infilling processes, encompassing sedimentary mechanisms (i.e. aeolian or aqueous) and upwelling of material from beneath the basin floor (i.e. mantle pluming, cryovolcanism, mud volcanism, springs). This study compares two such basins, Sputnik Planitia (1000 km diameter) on Pluto and Caloris Basin (1500 km diameter) on Mercury, both believed to have been infilled through upwelling from the basin floor, facilitated by reduced lithosphere thickness directly below. As Mercury and Pluto represent opposite ends of the planetary spectrum (small silicate planet vs icy dwarf planet), this comparative analysis aims to advance our understanding of impact-induced mechanisms and subsequent infilling.

Although their volume and thickness are comparable, their infill composition starkly contrast; nitrogen ice in Sputnik and basaltic lava in Caloris. This is due to the ice water-water ocean composition of Pluto’s lithosphere-mantle boundary and the rocky composition of Mercury’s. The infill of Sputnik is at least 3 km thick and is relatively flat. The perimeter of Sputnik is characterized by a smooth, radially asymmetrical, forebulge which has been retained in many places. In contrast, the infill within Caloris is at least 3.5 km thick and shows a highly variable topography, exhibiting high bulges that exceed the height of the basin rim, as well as a central depression. Both infills contain a plethora of deformational features such as faults, polygons, vents and mounds. Although each basin has their own unique geological history, comparing their deformational features (i.e. faults and bulge topography) provides particular insight into the intricate interplay of composition, gravity and volume in driving subsidence (whether faulting induced or isostatic) on planetary bodies.

Here we present the results from a topographical analysis utilizing a Monte Carlo statistical approach, and a morphological analysis of faults and fractures observed within infill and the basin surroundings. Both the perimeter bulge topography of Sputnik and the infill bulge topography of Caloris were analyzed by adopting equations for linear and central load flexure under various conditions (i.e. Young’s Elastic Modulus and Poisson ratio), to estimate the induced load required to deform them to their present topography. These areas can then be compared to specific structures on Earth such as lava domes and flexural bulges found in various tectonic provinces.

This work further refines the framework for interpreting the subsurface architecture (i.e. fault geometry, lithosphere thickness and nature of the mantle-lithosphere boundary) beneath these basins. It also provides insights into the relationship between magma and water/cryomagma pluming beneath deep basins (i.e. volcanism vs. cryovolcanism). Due to the imminent arrival of BepiColombo in Mercury’s orbit in 2025, categorizing and comparing these infilled basins will enhance our capacity to interpret the geophysical and topographical data expected from the Mercury Planetary Orbiter (MPO). We acknowledge support from the SIMBIO-SYS/Bepicolombo project under ASI-INAF agreement n. 2017-47-H1.

How to cite: Schmidt, G., Sepe, A., Galuzzi, V., and Palumbo, P.: Deformational histories of the massive infill within Sputnik Planitia (Pluto) and Caloris Basin (Mercury) : Implications for BepiColombo data interpretation and the relationship between the parameters which induce tectonic subsidence, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-20756, https://doi.org/10.5194/egusphere-egu24-20756, 2024.

Microbial Volatile Organic Compounds (mVOCs) are small organic molecules produced by microorganisms that readily evaporate at low temperatures. They have a number of functions, ranging from being waste products to modulating stress response and enhancing intra- and/or interspecies communication[1]. Furthermore, VOCs undergo complex chemical reactions in the atmosphere by reacting with hydroxyl radicals and nitrogen oxides, as well as forming secondary aerosols[2]. The production of mVOCs is influenced, among others, by changes in the environment. These molecules have the potential to be used as biomarkers in extreme environments to monitor the presence of life. They may also contribute to global element cycles in extreme environments, such as the sulfur cycle[3]. Lastly, they are also potential ways for extant life to influence the atmosphere of other planetary bodies.

This study aims to broaden our understanding of mVOCs in the High Arctic deserts of Northern Greenland, a terrestrial analogue of Mars-like planets characterized by low temperatures and low water availability. Three novel bacterial strains were isolated from Peary Land, northern Greenland: Oceanobacillus sp. and Nesterenkonia aurantiaca CMS1.6 from dry crust soil, and Arthrobacter sp. from permafrost. The three strains were grown at 0, 5 and 10% w/v NaCl. In the late exponential phase, the headspace was sampled and the volatiles were up-concentrated using Tenax tubes. Gas Chromatography – Mass Spectroscopy (GC-MS) was then used to analyse mVOCs in the samples. In a separate experiment, Proton Transfer Reaction Mass Spectroscopy (PTR-MS) was used to monitor the mVOC production of these strains over 72 hours, from the latent phase to the stationary phase.

Principal Component Analysis (PCA) of the mVOC profile revealed that each strain has a characteristic pattern, although the statistical effect of salt concentration is less clear. In particular, N. aurantiaca CMS1.6 produced large amounts of 2- and 3-methylbutanol under all conditions, which was not observed in the other strains. The real-time measurements also reveal different emission patterns for different compounds throughout the growth of the strains. These results highlight the potential of specific mVOCs as biomarkers in extreme environments, with potential applications in taxonomy, ecology, biotechnology and astrobiology.

[1] L. Weisskopf, S. Schulz, and P. Garbeva, “Microbial volatile organic compounds in intra-kingdom and inter-kingdom interactions,” Nat. Rev. Microbiol., vol. 19, no. 6, pp. 391–404, 2021, doi: 10.1038/s41579-020-00508-1.

[2] R. Atkinson, “Atmospheric chemistry of VOCs and NOx,” Atmos. Environ., vol. 34, no. 12, pp. 2063–2101, 2000, doi: https://doi.org/10.1016/S1352-2310(99)00460-4.

[3] D. J. Baumler, K.-F. Hung, K. C. Jeong, and C. W. Kaspar, “Production of methanethiol and volatile sulfur compounds by the archaeon ‘Ferroplasma acidarmanus,’” Extremophiles, vol. 11, no. 6, pp. 841–851, Nov. 2007, doi: 10.1007/s00792-007-0108-8.

How to cite: Salinas-García, M. Á., Roslund, K., Bygum Risom, M., Rinnan, R., and Priemé, A.: Extreme smells: Volatile Organic Compounds from Greenlandic bacteria as biomarkers, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-10372, https://doi.org/10.5194/egusphere-egu24-10372, 2024.

Silicates are the main constituent of volcanic terrains on terrestrial planets in the Solar system. On Earth, we know that volcanic terrains are constituted by lava flows and fragmented pyroclasts whose texture presents both glassy and crystalline phases. Understanding the influence of glass/crystal ratio on the spectral response of volcanic rocks is therefore focal to interpret remotely sensed spectra that are commonly used to interpret the geology of terrestrial planets. Thus, we performed spectral characterization of lab-made mafic volcanic products which were  synthesized in the PVRG labs with the aim to present different degrees of crystallinity.

Samples were synthesized  by mixing and melting oxides to resemble the composition of a Nakhlite meteorite. First we produced a homogeneous silicate glass (Nglass) which was then used to prepare three more samples by melting at 1500°C and then cooling down slowly (52-56 °C per hour) towards subliquidus temperatures of ca. 1200°C (N12), 1100°C (N11), and 1000°C (N10), respectively. Each sample stayed for 48 hours at the target temperature and was finally quenched in air.

SEM and XRPD analyses and Rietveld method quantitative phase analyses were performed to assess type and degree of crystallinity, showing how N11 and N10 present a similar mineralogical assemblage with ca. 30% of glass and crystal species including augite, magnetite, cristobalite and other minor phases similar to the mineralogical composition of a natural Nakhlite. Sample N12 presents less diverse mineralogy (augite and magnetite) and ca. 70% of glass. 

Bi-directional reflectance spectra was collected at room temperature in the 1-4.2 µm range considering a set of 3 incidence angles (i = 0°; 30°; 60°) and emergence (e) angles between -70° and 70° using the custom-made bidirectional reflectance spectro-goniometers SHINE at the Cold Surface Spectroscopy facility (CSS) of the IPAG laboratory in the frame of the Trans-National Access program, project number 21-EPN-FT1-025, of Europlanet 2024.

Spectral analyses show how, in the Visible and Near-Infrared, increasing crystallinity causes slopes of spectra to gradually shifts from positive for glasses towards flat-negative for crystalline material. The spectral features of the single mineral phases are barely distinguishable for N10 and N11, where spectra are flattened probably because of the presence of magnetite, whereas the spectral signature of Fe in augite is distinguishable for N12 located at ~0.9 and ~1.15 µm.
Changing observation geometry, reflectance values and spectral slope show important variations while the bands position remains unchanged. We observe important dependence of band and slope in correspondence of low phase (< 30°) angle and high phase angle (> 100°).

To identify distinctive features we used principal component analysis (PCA) obtaining four clusters in the PC space which are relatable to the four samples. K-means clustering was used to verify our clustering obtaining a very low level of misclassification, especially regarding Nglass.

These results provide further information on the spectral response of synthesized rock samples, especially for what concerns glass-bearing materials, that can be used for modeling of spectral information coming from volcanic rocky bodies in the Solar system.

How to cite: Pisello, A., Fastelli, M., Baroni, M., Schmitt, B., Beck, P., Zucchini, A., Petrelli, M., Comodi, P., and Perugini, D.: Spectral characterization of lab-made Nakhlitic rock powders: effects of crystal/glass ratio and acquisition geometry., EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-19432, https://doi.org/10.5194/egusphere-egu24-19432, 2024.

Introduction

Lonar crater in India offers important mineralogy insights into impact-related processes. One of the key minerals found within the crater is maskelynite, a high-pressure diaplectic glass formed by shock metamorphism during meteorite impacts (Xie et al. 2020). In this study, we conducted a Raman spectroscopy analysis on several samples of M-S4 shocked basalt (maskelynite-bearing from solid state shock pressures and not M-S5 through M-S7 in which labradorite is melted) collected from Lonar crater to identify maskelynite phenocrysts, contributing to our understanding of the crater's geology and the processes involved in maskelynite formation. The presence of maskelynite is an indicator of an intense shock event (Wright et al. 2011; Jaret et al. 2015).

Method

The method prepared thin M-S4 sample sections for Raman spectroscopy. Raman spectra used a red excitation laser (785 nm), 20X objective lens, 10 s exposure time, and 10% laser power. Spectra were obtained from various 30-45 micron maskelynite phenocrysts within M-S4 samples, while smaller needles were ignored. Baselines were subtracted, and an average Raman spectrum was generated by combining 10 individual spectra. The ~570 cm-1 peak is attributed to maskelynite. (Fritz et al. 2005; Kanemaru, et al. 2020).

Discussion

The feature at 576 cm^-1 on the averaged Raman spectrum of Lonar maskelynite in basalts shocked ~20-40 GPa is particularly noteworthy (Fig.1). The presence of maskelynite in FTIR images of shocked soil from Lonar has been shown by Wright and Michalski (2024). Figures 4 and 9 of Wright et al. (2011) investigated the TIR emission spectrum of Lonar maskelynite.

Figure 1. The average Raman spectrum of phenocrysts of maskelynite in MS-4 Lonar samples.

The study connects Lonar crater's maskelynite to Martian meteorites, enhancing understanding of meteorite impacts on Mars' mineral composition and geologic history (Fritz et al. 2005; El Goresy et al. 2013). The findings link Lonar crater's maskelynite to Martian meteorites, providing vital insights into meteorite impacts' effects on Mars' mineral composition and geologic history.

Conclusion

Lonar crater is a great analog for studying Martian surface materials and processes due to its similarities with Mars' impact craters. This study successfully characterized maskelynite phenocrysts within M-S4 Lonar crater samples using Raman spectroscopy (Xie et al. 2021). The average Raman spectra offer crucial insights into the composition and formation of maskelynite. The research highlights Raman spectroscopy's significance as a dependable method for mineral analysis in impact-related samples, with potential applications at meteorite impact sites globally.

References:

El Goresy, A., et al. 2013. G.C.A, 101, pp.233-262.

Fritz, J., et al. 2005. Antarctic Meteorite Research, Vol. 18, p. 96, 18, p.96.

Jaret, S.J., et al. 2015. J.  Geophysical Research: Planets, 120 (3), pp.570-587.

Kanemaru, R., et al. 2020. Polar Science, 26, p.100605.

Wright, S.P., et al. 2011. J. G.R.P. 116 (E9).

Wright, S.P. and J.R. Michalski, 2024, JGR-Planets, doi: 10.1029/2023JE007913.

Xie, T., et al. 2020. M & P Science, 55 (7), pp.1471-1490.

Xie, T., et al. 2021. M & P Science, 56 (9), pp.1633-1651.

How to cite: Tanbakouei, S., Wright, S. P., and Michalski, J. R.: Raman Spectroscopy Analysis of Maskelynite in M-S4 Lonar crater Samples, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-18034, https://doi.org/10.5194/egusphere-egu24-18034, 2024.

The surface of Mercury is subject to space weathering that complicates remote sensing data analysis [1]. Constraining the effect of space weathering is necessary to reconstruct the geological history and surface evolution of the planet using spectral data. Previous studies highlighted the necessity to deeper investigate spectral changes induced by ion irradiation simulating solar wind reaching Mercury [1, 2].

We present an experimental study performed on Mercury’s volcanic surface analogues. We used 20 keV He⁺with fluences up to 5.10¹⁷ ions/cm² to simulate ion irradiation reaching the surface. Terrestrial ultramafic lava already identified as good analogues for Mercury were used [3, 4, 5]: a boninite, a basaltic komatiite and a komatiite. Spectra were acquired in the VMIR wavelengths range between 0.4 and 16 μm. Ion irradiations were performed with the SIDONIE electromagnetic isotope separator (CSNSM, Orsay, France) [6] interfaced with the INGMAR (IrradiatioN de Glaces et Météorites Analysées par Réflectance VIS-IR, IAS-CSNSM, Orsay, France) setup [7]. Using INGMAR, we performed VNIR in-situ reflectance spectroscopy measurements. MIR analysis were conducted at the Synchrotron SOLEIL (France) using the SMIS beamline (Spectroscopy and Microscopy in the Infrared using Synchrotron) [8]. 

Several spectral modifications induced by irradiation are observed. In the VNIR samples show an exponential darkening, a reddening and a flattening of spectra. Above a certain irradiation dose, the darkening reaches a plateau while the reddening and flattening do not show any definable trend. After a certain irradiation dose/time exposure spectral differences among different units on Mercury will be limited. In the MIR we observe a red-shift of Reststrahlen bands. The Christiansen feature is red or blue shifted according to the irradiation dose. Spectral modifications in the VMIR are closely influenced by the composition and will likely participate in the origin of spectral heterogeneities on Mercury.

This work provides ground-truth data for the future ESA/JAXA/BepiColombo observations [9]. VMIR spectral modifications induced by ion irradiation simulated in laboratory will be used for future SIMBIO-SYS (Spectrometer and Imaging for MPO BepiColombo Integrated Observatory SYStem) [10] and MERTIS (Mercury Radiometer and Thermal Infrared Spectrometer) [11] data analysis.

[1] Domingue, D. L. et al. (2014), Space science Reviews, 181, 121-214. [2] Jäggi, N. et al. (2021), Icarus, 365, 114492. [3] Carli, C. et al. (2013). [4] Mari, N. et al. (2023), Planetary and Space Science, 105764. [5] Serrano, L. M. (2009). [6] Chauvin, N. et al. (2004), Nuclear Instruments and Methods in Physics Reasearch Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, 521(1), 149-155. [7] Lantz, C. et al. (2017), Icarus, 285, 43-57. [8] Dumas, P. et al. (2006), Infrared Physics & technology, 49(1-2), 152-160. [9] Benkhoff, J. et al. (2021), Space science review, 217(8),90. [10] Cremonese, G. et al. (2021), Space science review, 216, 1-78. [11] Hiesinger, H. et al. (2020), Space science reviews, 216, 1-37.

How to cite: Caminiti, E., Lantz, C., Besse, S., Brunetto, R., Carli, C., Serrano, L., Mari, N., Vincendon, M., and Doressoundiram, A.: Effects of ion irradiation on Mercury terrestrial analogues in the visible to mid-infrared, EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-5197, https://doi.org/10.5194/egusphere-egu24-5197, 2024.

The study of astrobiology, in particular testing concepts for searching for biosignatures in extraterrestrial environments or conducting experiments for survivability of microorganisms in extraterrestrial materials and conditions, but also the branch of science and engineering focusing on testing instruments in planetary environments or identifying materials and energy resources (ISRU), both require analogue studies with simulated extraterrestrial materials. Thus, the development of accurate and representative simulant regoliths and soils is crucial [1]. In this study, we present new Martian simulants that have been developed to expand the suite of available lithologies and compositions, while also try to address limitations of previous simulants.

Extensive research has been conducted by our team to analyze the chemical and physical properties of martian surface datasets, including their mineralogy, grain size distribution, and chemical composition. [2], [5], [6]. Thus, our new Martian simulants have been developed to better represent the unique geological and mineralogical features of specific locations of the martian surface. We have used XRD, SEM-EDS, and LIBS analysis to verify the accuracy of our simulants to the reference target compositions. The additions of those new simulants, and their characterisation steps, provide valuable insights for developing even more accurate simulants of the varied geological and environmental conditions of current and early Mars.

Our approach to simulant fidelity and quality involves firstly the reproduction of the accurate mineralogy, which can finally be expressed in chemical terms using an arithmetic quality value, the Figure of Merit (FoM) [3],[4]. This is a standardized fidelity compositional comparison of the oxide differences with the compositions of the reference datasets. In this FoM the grain size distribution and other parameters are not included. The same FoM system is also used to compare our different simulant batches in order to ensure consistency in their production. A constant increase in FoM is achieved in each consequent batch of simulants produced in our lab, with values exceeding 90% of FoM. These values provide confidence in our methods since it provides a way to increase the fidelity of the simulants.

In this presentation we will discuss the methodology and tools we use to achieve the above results, aiming to more representative lithologies, compositions and textures. For each new simulant, we also address the potential impact on specific fields of research, such as their compatibility for either ISRU research, or for astrobiological investigations. We envisage that with further research we can cover the requirements for simulants of new research studies, addressing topics such as planetary evolution and habitability.

1. G. H. Peters et al. (2008), Icarus 197, 470-479.
2. H.-A. Stavrakakis et al. (2022), EPSC2022.
3. C. Schrader et al. (2009), 47th AIAA Aerospace Sciences Meeting Including the New Horizons Forum and Aerospace Exposition, p 755.
4. L. E. Fackrell, et al. (2021). Icarus 354, 114055. 
5. D. Argyrou et al. (2023), EANA23. “Characteristics of Greek Martian and Lunar Simulants: Insights from the initial development”
6. Georgiou C. et al. (2023), EANA23. “OxR: A novel device for Reactive Oxygen Species (ROS) detection for astrobiology and planetary research”

How to cite: Argyrou, D., Stavrakakis, H.-A., and Chatzitheodiridis, E.: Synthesizing Mars: Advancements in Simulant Lithology for Astrobiological and ISRU Studies , EGU General Assembly 2024, Vienna, Austria, 14–19 Apr 2024, EGU24-12957, https://doi.org/10.5194/egusphere-egu24-12957, 2024.