Stephanie Werner

• Wong, E. W.; Werner, Stephanie; Kirchoff, M. R. & Brasser, Ramon (2026). The Enceladian crater production function. Icarus (New York, N.Y. 1962). ISSN 0019-1035. 461, p. 1–18. doi: 10.1016/j.icarus.2026.117300. Full text in Research Archive
• Mamonova, E.; Herbst, K.; Kofman, V.; Ozgurel, Ozge; Kowalski, A. F. & Wedemeyer, S. [Show all 7 contributors for this article] (2026). Stellar-flare-driven evolution of primordial early exo-Earth atmospheres: Insights from the young M dwarf flare model. Astronomy and Astrophysics (A & A). ISSN 0004-6361. 710. doi: 10.1051/0004-6361/202558763. Full text in Research Archive Show summary

  Context . M dwarfs are key targets for terrestrial exoplanet studies, with prospects for atmospheric spectroscopy. However, strong stellar magnetic activity and frequent flaring require modelling efforts to assess their impact on planetary atmospheres. Aims . We investigated one year of atmospheric chemical evolution of a young exo-Earth orbiting an active M dwarf by coupling our young M dwarf flare (YMDF) model of stellar activity with the photochemical kinetic code VULCAN. Methods . The YMDF model provides time-resolved spectral energy distributions for high- and low-energy electron beam–driven flares, which are used as external radiative inputs to VULCAN to compute the time-dependent photochemistry and kinetics for different primordial atmospheric scenarios. Results . We present the impact of stellar flares on atmospheres with a varying water vapour content, ranging from a plausible primordial atmosphere with solar abundances (representative of a planet-forming region in a dissipating protoplanetary disk) to an extreme water-steam atmosphere with other species reduced to trace abundances. This was explored across several configurations: variable flux in the YMDF model, the previous model representing an active but older M dwarf with 10 or 400K additional bottom boundary heat flux, and a constant stellar flux model. Conclusions . Our study suggests that compared to the previous model, the YMDF model produces synthetic flares that exert significantly greater stress on primordial atmospheres, regardless of the water-vapour content. Increased activity and prevalence of mid-size flares has the potential to induce permanent changes in atmospheric mixing ratios, especially in species with low abundances.

• Mamonova, Elena; Kowalski, A.F.; Herbst, Konstantin; Wedemeyer, Sven & Werner, Stephanie C. (2026). Young M-dwarfs flare activity model: Towards better exoplanetary atmospheric characterisation. Astronomy and Astrophysics (A & A). ISSN 0004-6361. 705. doi: 10.1051/0004-6361/202556844. Full text in Research Archive Show summary

  Context. Stellar flares can significantly influence the atmospheres and habitability of orbiting exoplanets, especially around young and active M dwarfs. Understanding the temporally and spectrally resolved activity of such stars is essential for assessing their impact on planetary environments. Aims. We aim to examine in detail state-of-the-art concepts of flare models to identify what is missing in our understanding of energy deposition during the flare event. By comparing synthetic and observed flare spectra, we seek to determine the modelling frameworks best suited for representing flare energetics and spectral far-ultraviolet features while providing a foundation for investigating flare impacts on exoplanet atmospheres. Methods. In this work, we built the Young M dwarf flare (YMDF) model utilising the combination of radiative-hydrodynamic (RHD) stellar atmosphere models with a high- and low-energy electron beam and corresponding synthetic observables. These models are based on physical principles and were validated with solar and stellar observations. Results. The newly developed YMDF model reproduces the observed continuum rise in both the TESS photometric band and the FUV-A spectral range. Furthermore, the flare distributions generated within this framework show consistency with those observed in our sample of stars. Conclusions. We have developed the YMDF model as a tool to reproduce the time-dependent spectra of flaring young M dwarfs, providing a physically motivated description of their spectral and temporal evolution during flare events.

• Mamonova, Elena; Shan, Yutong; Kowalski, Adam F.; Wedemeyer, Sven & Werner, Stephanie (2025). Flare frequency in M dwarfs belonging to young moving groups. Astronomy and Astrophysics (A & A). ISSN 0004-6361. 700. doi: 10.1051/0004-6361/202554614. Full text in Research Archive Show summary

  Context. M stars are preferred targets for upcoming studies of terrestrial exoplanets aimed at obtaining their atmosphere spectra over the next decade. However, M dwarfs have long been known for their strong magnetic activity and the ability to frequently produce optical and broadband emission flares. Aims. We aim to characterise the flaring behaviour of young M dwarfs in the temporal, spectral, and energy dimensions, as well as examine the stellar parameters governing this behaviour. In this way, we aim to improve our understanding of the energy and frequency of the flare events capable of shaping the exoplanet atmosphere. Methods. Members of young moving groups (YMGs) provide a unique age-based perspective on stellar activity. By examining their flare behaviour in conjunction with rotation, mass, and Hα data, we can obtain a comprehensive understanding of flare-activity drivers in young stars. Results. We demonstrate that young stars sharing similar stellar parameters could also exhibit a broad range of flare frequency distributions. We also find that the flare behaviour shows indications of difference between optical and far ultraviolet (FUV). We propose that the period of rotation (and not the age of the star) can serve as a good proxy for assessing flaring activity. Furthermore, we recommend that instead of a simple power law for describing the flare frequency distribution, a piecewise power law can be used to describe mid-size and large flare distributions in young and active M dwarfs. Conclusions. Using known periods of rotation and fine-tuned power laws governing the flare frequency, we can produce a realistic sequence of flare events to study whether the atmosphere of small exoplanets orbiting M dwarf could withstand such activity until the emergence of life.

• Brasser, Ramon; Wong, Emily W. & Werner, Stephanie (2025). The current impact rate on the regular satellites of Jupiter, Saturn, and Uranus. Astronomy and Astrophysics (A & A). ISSN 0004-6361. 695. doi: 10.1051/0004-6361/202453433. Full text in Research Archive Show summary

  Context. The impact and cratering rates onto the regular satellites of the giant planets are subject to great uncertainties. Aims. We aim to compute the impact rates for objects with a diameter Di > 1 km onto the regular satellites of Jupiter, Saturn, and Uranus using dynamical simulations of the evolution of the outer Solar System coupled with the best estimates of the current population of objects beyond Neptune, and their size-frequency distribution. Methods. We analyse the last 3.5 billion years of evolution of the outer Solar System from our database of simulations and combine this with observational constraints of the population beyond Neptune to compute the flux of objects entering the Centaur region. The initial conditions of these simulations resemble the current population. We obtain an improved estimate of the impact probability of a Centaur with the satellites from enacting simulations of planetesimals flying past the satellites on hyperbolic orbits, which agree with literature precedents. Results. Our impact rate of objects Di > 1 km with Jupiter is 0.001 yr−1, which is 3–6 times lower than previous estimates. Both our impact probabilities with the satellites scaled to the giant planets and leakage rate of objects from beyond Neptune into the Centaur region are consistent with earlier literature estimates. However, our absolute impact probabilities with the giant planets are lower. We attribute this difference to whether the impact probabilities are computed over the whole age of the Solar System including planet migration, or over a shorter interval closer to the present. Conclusions. Our lower impact rate compared to earlier literature estimates is due to basing our results on the flux of objects coming in from beyond Neptune rather than relying on the current observed impact rate with Jupiter. We stress the importance of clearly stating all parameters and assumptions in future studies to enable meaningful comparisons.

• Hatalova, Petra; Brodholt, John Peter; Brasser, Ramon; Shan, Yutong & Werner, Stephanie C. (2025). The compositional diversity of rocky exoplanets around K-dwarf stars. Astronomy and Astrophysics (A & A). ISSN 0004-6361. 694. doi: 10.1051/0004-6361/202451070. Full text in Research Archive Show summary

  Context. The mass-radius distribution of currently known exoplanets suggests a fascinating variety in terms of their chemical compositions. Still, the interior structures and compositions of rocky exoplanets are essentially inaccessible to observations. Here, we present a model that combines planet formation simulations with equilibrium condensation models to estimate the interior composition and structure of exoplanets around K-dwarf stars. Aims. In a previous study, we reproduced the observed population of close-in super-Earths around K-dwarf stars with suitable initial conditions. However, the masses and radii of these simulated planets are not self-consistent, since the radius information is postprocessed based on an assumed constant average density (3 g cm−3). In this work, we have incorporated compositions into the N-body simulations using the chemistry of the protoplanetary disk from equilibrium condensation sequences, together with thermodynamics of the various mineral phases. This has allowed us to develop models of likely interior structures, bulk densities, and, thus, radii for rocky exoplanets. Methods. We selected the outcomes of ten N-body simulations around a 0.8 M⊙ star that best reproduced the observed population. We employed stellar abundances from six K-dwarf stars with a range of metallicities. Based on the condensation sequence and the temperature-pressure profile of a disk, we assigned bulk elemental compositions to planetesimals and then tracked materials accreted onto planets during their formation. Results. We have obtained a set of planets with more realistic radii determinations than those purely based on one preset density for all bodies. We formed various types of planets: i) Ca- and Al-rich(er), ii) Mg-depleted, iii) fully oxidized core-less planets, iv) planets similar to Earth or Mars in composition and core size, and v) planets with different core mass fractions (from significantly smaller than the Martian core to significantly larger than the Earth’s core); however, we do not have Mercury-like planet with a huge core.

• Rauer, Heike; Aerts, Conny; Cabrera, Juan; Deleuil, Magali; et, al., including: & Erikson, Anders [Show all 847 contributors for this article] (2025). The PLATO mission. Experimental astronomy (Print). ISSN 0922-6435. 59. doi: 10.1007/s10686-025-09985-9. Full text in Research Archive Show summary

  PLATO (PLAnetary Transits and Oscillations of stars) is ESA’s M3 mission designed to detect and characterise extrasolar planets and perform asteroseismic monitoring of a large number of stars. PLATO will detect small planets (down to <2R) around bright stars (<11 mag), including terrestrial planets in the habitable zone of solar-like stars. With the complement of radial velocity observations from the ground, planets will be characterised for their radius, mass, and age with high accuracy (5%, 10%, 10% for an Earth-Sun combination respectively). PLATO will provide us with a large-scale catalogue of well-characterised small planets up to intermediate orbital periods, relevant for a meaningful comparison to planet formation theories and to better understand planet evolution. It will make possible comparative exoplanetology to place our Solar System planets in a broader context. In parallel, PLATO will study (host) stars using asteroseismology, allowing us to determine the stellar properties with high accuracy, substantially enhancing our knowledge of stellar structure and evolution. The payload instrument consists of 26 cameras with 12cm aperture each. For at least four years, the mission will perform high-precision photometric measurements. Here we review the science objectives, present PLATO‘s target samples and fields, provide an overview of expected core science performance as well as a description of the instrument and the mission profile towards the end of the serial production of the flight cameras. PLATO is scheduled for a launch date end 2026. This overview therefore provides a summary of the mission to the community in preparation of the upcoming operational phases.

• Fawdon, Peter; Orgel, Csilla; Adeli, Solmaz; Balme, Matt; Calef, Fred J. & Davis, Joel M. [Show all 80 contributors for this article] (2024). The high-resolution map of Oxia Planum, Mars; the landing site of the ExoMars Rosalind Franklin rover mission. Journal of Maps. 20(1). doi: 10.1080/17445647.2024.2302361. Full text in Research Archive Show summary

  This 1:30,000 scale geological map describes Oxia Planum, Mars, the landing site for the ExoMars Rosalind Franklin rover mission. The map represents our current understanding of bedrock units and their relationships prior to Rosalind Franklin’s exploration of this location. The map details 15 bedrock units organised into 6 groups and 7 textural and surficial units. The bedrock units were identified using visible and near-infrared remote sensing datasets. The objectives of this map are (i) to identify where the most astrobiologically relevant rocks are likely to be found, (ii) to show where hypotheses about their geological context (within Oxia Planum and in the wider geological history of Mars) can be tested, (iii) to inform both the long-term (hundreds of metres to ∼1 km) and the short-term (tens of metres) activity planning for rover exploration, and (iv) to allow the samples analysed by the rover to be interpreted within their regional geological context.

• Torsvik, Trond Helge; Royer, Dana L.; Marcilly, Chloe M. & Werner, Stephanie C. (2024). User-friendly carbon-cycle modelling and aspects of Phanerozoic climate change. Applied Computing and Geosciences. 23. doi: 10.1016/j.acags.2024.100180. Full text in Research Archive Show summary

  Carbon-cycle modelling is essential for testing the main carbon sources and sinks as climate forcings, and we introduce and describe GEOCARB_NET, a graphical user interface for the geologic carbon and sulfur cycle model GEOCARBSULFvolc. The software system is menu-driven, user-friendly, and the user is never far removed from the basic input parameters from which atmospheric CO2 and O2 concentrations can be derived. GEOCARB_NET is supplied with several published models and the user can easily test and refine these models with different parametrizations. GEOCARB_NET also contains libraries of models and proxy data, which easily can be compared with each other. Our examples focus on how to use GEOCARB_NET in the context of Phanerozoic climate change and highlights how certain key input parameters can seriously affect reconstructed CO2 levels.

• Mamonova, Elena; Shan, Yutong; Hatalova, Petra & Werner, Stephanie C. (2024). Planets similar in size are often dissimilar in interior. Astronomy and Astrophysics (A & A). ISSN 0004-6361. 685. doi: 10.1051/0004-6361/202347049. Full text in Research Archive Show summary

  The number of discovered exoplanets now exceeds 5500 allowing statistical analyses of planetary systems. Multi-planet systems are mini-laboratories of planet formation and evolution, and analysing their system architectures can help us to constrain the physics of these processes. Recent works have found evidence of significant intrasystem uniformity in planet properties such as radius, mass, and orbital spacing, collectively termed ‘peas in a pod’ trends. In particular, correlations in radius and mass have been interpreted as implying uniformity in planet bulk density and composition within a system. However, the samples used to assess trends in mass tend to be small and biased. In this paper, we re-evaluate correlations in planet properties in a large sample of systems with at least two planets for which mass and radius have been directly measured, and therefore bulk density can be calculated. Our sample was assembled using the most up-to-date exoplanet catalogue data, and we compute the relevant statistics while using a procedure to ‘weight’ the data points according to measurement precision. We find a moderate correlation in radius and a weak correlation in the densities of adjacent planets. However, masses of neighbouring planets show no overall correlation in our main sample and a weak correlation among pairs of planets similar in size or pairs restricted to Mp<100 M⊕, Rp<10 R⊕. Similarly, we show that the intrasystem dispersion in radius is typically less than that in mass and density. We identify ranges in stellar host properties that correlate with stronger uniformity in pairs of adjacent planets: low Teff for planet masses, and low metallicity and old age for planet densities. Furthermore, we explore whether peas in a pod trends extend into planet compositions or interior structures. For small neighbouring planets with similar radii, we show that their masses and interior structures are often disparate, indicating that even within the same system, similarity in radii is not necessarily a good proxy for similarity in composition or the physical nature of the planets.

• Wong, E.W.; Brasser, R.; Werner, Stephanie C. & Kirchoff, M.R. (2023). Saturn's ancient regular satellites. Icarus (New York, N.Y. 1962). ISSN 0019-1035. 406. doi: 10.1016/j.icarus.2023.115763. Full text in Research Archive
• Prieur, Nils Charles; Amaro, Brian; Gonzalez, Emiliano; Kerner, Hannah; Medvedev, Sergei & Rubanenko, Lior [Show all 10 contributors for this article] (2023). Automatic Characterization of Boulders on Planetary Surfaces From High-Resolution Satellite Images. Journal of Geophysical Research (JGR): Planets. ISSN 2169-9097. 128(11). doi: 10.1029/2023JE008013. Full text in Research Archive Show summary

  Abstract Boulders form from a variety of geological processes, which their size, shape, and orientation may help us better understand. Furthermore, they represent potential hazards to spacecraft landing that need to be characterized. However, mapping individual boulders across vast areas is extremely labor‐intensive, often limiting the extent over which they are characterized and the statistical robustness of obtained boulder morphometrics. To automate boulder characterization, we use an instance segmentation neural network, Mask R‐CNN, to detect and outline boulders in high‐resolution satellite and aerial images. Our neural network, BoulderNet, was trained from a data set of &gt;33,000 boulders in &gt;750 image tiles from Earth, the Moon, and Mars. BoulderNet not only correctly detects the majority of boulders in images but also identifies the outline of boulders with high fidelity, achieving average precision and recall values of 72% and 64% relative to manually digitized boulders from the test data set, when only detections with intersection‐over‐union ratios &gt;50% are considered valid. These values are similar to those obtained from human mappers. On Earth, equivalent boulder diameters, aspect ratios, and orientations extracted from predictions were benchmarked against ground measurements and yield values within ±15%, ±0.20, and ±20° of their ground‐truth values, respectively. BoulderNet achieves better boulder detection and characterization performance relative to existing methods, providing a versatile open‐source tool to characterize entire boulder fields on planetary surfaces.

• Hatalova, Petra; Brasser, R.; Mamonova, Elena & Werner, Stephanie C. (2023). Forming rocky exoplanets around K-dwarf stars. Astronomy and Astrophysics (A & A). ISSN 0004-6361. 676. doi: 10.1051/0004-6361/202346332. Full text in Research Archive Show summary

  Context. New space telescopes, such as the upcoming PLATO mission, aim to detect and study thousands of exoplanets, especially terrestrial planets around main-sequence stars. This motivates us to study how these planets formed. How multiple close-in super-Earths form around stars with masses lower than that of the Sun is still an open issue. Several recent modeling studies have focused on planet formation around M-dwarf stars, but so far no studies have focused specifically on K dwarfs, which are of particular interest in the search for extraterrestrial life. Aims. We aim to reproduce the currently known population of close-in super-Earths observed around K-dwarf stars and their system characteristics. Additionally, we investigate whether the planetary systems that we form allow us to decide which initial conditions are the most favorable. Methods. We performed 48 high-resolution N -body simulations of planet formation via planetesimal accretion using the existing GENGA software running on GPUs. In the simulations we varied the initial protoplanetary disk mass and the solid and gas surface density profiles. Each simulation began with 12 000 bodies with radii of between 200 and 2000 km around two different stars, with masses of 0.6 and 0.8 M ⊙ . Most simulations ran for 20 Myr, with several simulations extended to 40 or 100 Myr. Results. The mass distributions for the planets with masses between 2 and 12 M ⊕ show a strong preference for planets with masses M p &lt; 6 M ⊕ and a lesser preference for planets with larger masses, whereas the mass distribution for the observed sample increases almost linearly. However, we managed to reproduce the main characteristics and architectures of the known planetary systems and produce mostly long-term angular-momentum-deficit-stable, nonresonant systems, but we require an initial disk mass of 15 M ⊕ or higher and a gas surface density value at 1 AU of 1500 g cm −2 or higher. Our simulations also produce many low-mass planets with M &lt; 2 M ⊕ , which are not yet found in the observed population, probably due to the observational biases. Earth-mass planets form quickly (usually within a few million years), mostly before the gas disk dispersal. The final systems contain only a small number of planets with masses M p &gt; 10 M ⊕ , which could possibly accrete substantial amounts of gas, and these formed after the gas had mostly dissipated. Conclusions. We mostly manage to reproduce observed K-dwarf exoplanetary systems from our GPU simulations.

• Werner, Stephanie; Bultel, Benjamin Gabriel Rene & Rolf, Tobias (2023). Review and Revision of the Lunar Cratering Chronology – Lunar Time Scale Part 2. The Planetary Science Journal (PSJ). 4(8). doi: 10.3847/PSJ/acdc16. Full text in Research Archive Show summary

  Abstract Times and rates of planetary surface-modifying processes are crucial for the sequence and correlation of events on planetary bodies. For most planetary surfaces, superposition principles and crater densities are commonly used methods to collect relative age information. Lunar-based cratering-chronology models, which pair crater densities and sample ages from several lunar landing and sampling sites, calibrate the relative age information in absolute time. Here, we propose calibration pairs based on new crater statistics and spectrally supported sample-age assignments for the lunar cratering-chronology model. The resulting model reflects modern high-precision, radiometric ages, compositional and spectral information, and an up-to-date crater-production function. This revision supports a crater-forming projectile flux with monotonic decay, similar to previous standard models, but of distinctively lower flux. This originates from lower crater densities identified in spectrally and morphologically defined reference units, and from assigning more precise sample ages accounting for spectral resemblance between reference unit and sample. The observed maximal values for crater densities and ages provide the oldest and most densely cratered calibration pair. Because of the nature of highland samples, age constraints for the Luna 20 and Apollo 16 sampling sites remain challenging, which restricts the confidence in times for individual basin-formation events older than Orientale Basin. The new cratering-chronology model, when transferred to other planetary bodies, would cause aging of the surfaces, because of the lower overall flux.

• Bultel, Benjamin Gabriel Rene & Werner, Stephanie C. (2023). Sample-based Spectral Mapping around Landing Sites on the Moon—Lunar Timescale Part 1. The Planetary Science Journal (PSJ). 4(146). doi: 10.3847/PSJ/acdc15. Full text in Research Archive Show summary

  Abstract Studying the geology of a terrestrial body and its evolution requires being able to set up a chronology. Crater statistics is a powerful tool to do so. However, calibration of this method, which is derived on the Moon, requires properly defined geological units, large enough for reliable crater statistics, and dated samples representative of these geological units. Yet, little effort has been put into choosing a representative set of lunar mission units and samples based on spectral information. Therefore, accuracy and precision of so-called cratering-chronology models remain limited. Here, we analyzed near-infrared orbital data to suggest a geological unit as a reference unit for Apollo 11, 12, 14–17 and Luna 16, 20, and 24 landing sites. We used near-infrared spectral information from orbital data and laboratory measurements to identify the set of samples that is the most representative of the landing-site reference units. We now provide spectrally constrained reference units, for which crater frequencies can be derived, and our sample recommendation will assign the reference age for updating the currently existing cratering-chronology models. We highlight that determining a reference geological unit in the highlands of the Moon is challenging because of the very nature of the terrain, while it is more straightforward for mare units. However, ejecta presence on these mare units comprises solvable challenges.

• Wu, Bo; Wang, Yiran; Werner, Stephanie C.; Prieur, Nils Charles & Xiao, Zhiyong (2022). A Global Analysis of Crater Depth/Diameter Ratios on the Moon. Geophysical Research Letters. ISSN 0094-8276. 49(20). doi: 10.1029/2022GL100886. Full text in Research Archive
• Werner, Stephanie; Bultel, Benjamin Gabriel Rene; Rolf, Tobias & Fernandes, Vera Assis (2022). Orientale Ejecta at the Apollo 14 Landing Site Implies a 200-million-year Stratigraphic Time Shift on the Moon. The Planetary Science Journal (PSJ). 3(3). doi: 10.3847/PSJ/ac54a6. Full text in Research Archive Show summary

  Abstract Detailed spectral mapping, cratering statistics, and impact basin ejecta column estimates document a new and very different stratigraphic relationship for the Apollo 14 landing site. We observe a resurfacing event in the crater size–frequency distribution in agreement with a single blanketing layer. Using the crater size–frequency distribution, we determine two relative ages (cumulative crater frequencies) that match those observed for the Imbrium and Orientale basins, respectively. The pattern and strength of resurfacing and morphological distinction by spectral features suggest the top layer to be about 10–25 m thick. We propose that this top layer at the Apollo 14 landing site is Orientale basin ejecta above Imbrium basin ejecta. Such stratigraphy reattributes the (majority of) Apollo 14 samples to Orientale rather than to Imbrium basin and implies that Orientale basin is about 3.92 Gyr old, 200 million years older than previously suggested. The youngest lunar basin thus formed at the onset, rather than amid, of recorded mare volcanism. This time shift also changes constraints on early planetary and solar system processes, such as the intensity of impact bombardment, and pleads for revision of the crater-statistics-based surface ages of other planetary bodies.

• Loizeau, Damien; Pilorget, Cédric; Poulet, François; Lantz, Cateline; Bibring, Jean-Pierre & Hamm, Vincent [Show all 11 contributors for this article] (2022). Planetary Terrestrial Analogues Library Project: 3. Characterization of Samples with MicrOmega. Astrobiology. ISSN 1531-1074. 22(3), p. 263–292. doi: 10.1089/ast.2020.2420. Full text in Research Archive
• Veneranda, Marco; Lopez-Reyes, Guillermo; Sanchez, Elena Pascual; Krzesinska, Agata Magdalena; Manrique-Martinez, Jose Antonio & Sanz-Arranz, Aurelio [Show all 15 contributors for this article] (2021). ExoMars Raman Laser Spectrometer: A Tool to Semiquantify the Serpentinization Degree of Olivine-Rich Rocks on Mars. Astrobiology. ISSN 1531-1074. 21(3), p. 307–322. doi: 10.1089/ast.2020.2265. Full text in Research Archive
• Helled, Ravit; Werner, Stephanie C.; Dorn, Caroline; Guillot, Tristan; Ikoma, Masahiro & Ito, Yuichi [Show all 13 contributors for this article] (2021). Ariel planetary interiors White Paper. Experimental astronomy (Print). ISSN 0922-6435. doi: 10.1007/s10686-021-09739-3. Full text in Research Archive Show summary

  Abstract The recently adopted Ariel ESA mission will measure the atmospheric composition of a large number of exoplanets. This information will then be used to better constrain planetary bulk compositions. While the connection between the composition of a planetary atmosphere and the bulk interior is still being investigated, the combination of the atmospheric composition with the measured mass and radius of exoplanets will push the field of exoplanet characterisation to the next level, and provide new insights of the nature of planets in our galaxy. In this white paper, we outline the ongoing activities of the interior working group of the Ariel mission, and list the desirable theoretical developments as well as the challenges in linking planetary atmospheres, bulk composition and interior structure.

• Kulakov, Evgeniy; Torsvik, Trond Helge; Doubrovine, Pavel V.; Slagstad, Trond; Ganerød, Morgan & Silkoset, Petter [Show all 7 contributors for this article] (2021). Jurassic fast polar shift rejected by a new high-quality paleomagnetic pole from southwest Greenland. Gondwana Research. ISSN 1342-937X. 97, p. 240–262. doi: 10.1016/j.gr.2021.05.021. Full text in Research Archive Show summary

  A selective compilation of paleomagnetic data from North America indicates that a vast amount of rapid polar motion occurred in Late Jurassic time. The over 30° polar shift that accumulated during a relatively short time interval (~160–145 Ma) suggests an episode of fast true polar wander (TPW) and was referred to as the Jurassic “monster polar shift” by some workers. However, this rapid TPW event is not supported by paleomagnetic data on a global scale. Here, we scrutinize the Jurassic apparent polar wander path (APWP) by virtue of a new paleomagnetic and 40Ar/39Ar geochronology study of Mesozoic coast-parallel dykes exposed in southwest Greenland. Combined with existing geochronological data, our results show that the dykes were emplaced during a prolonged period centered at 147.6 ± 3.4 Ma (2σ). A primary nature of the characteristic remanent magnetization is supported by multiple positive baked contact tests and a reversal test. The paleomagnetic pole calculated from 40 site-mean paleomagnetic directions is located at Plat = 69.3°S, Plong = 5.0°E (A95 = 4.6°), or at Plat = 73.9°S and Plong = 0.4°E when reconstructed to North America. Our new high-quality paleomagnetic pole and an updated global APWP do not support the fast Jurassic polar shift but instead indicate steady polar motion with moderate rates of about 0.7°/Myr. The new pole effectively reduces the mismatch between the APWPs for Laurentia and Europe. Our critical reassessment of the monster polar shift indicates that it may be an artifact of paleomagnetic and geochronological data that were previously used to argue for its existence.

• Brasser, R.; Mojzsis, S. J.; Werner, Stephanie C. & Abramov, Oleg (2021). A new estimate for the age of highly-siderophile element retention in the lunar mantle from late accretion. Icarus (New York, N.Y. 1962). ISSN 0019-1035. 361. doi: 10.1016/j.icarus.2021.114389. Full text in Research Archive
• Dypvik, Henning; Hellevang, Helge; Krzesinska, Agata Magdalena; Sætre, Christian; Viennet, Jean-Christophe & Bultel, Benjamin Gabriel Rene [Show all 13 contributors for this article] (2021). The Planetary Terrestrial Analogues Library (PTAL) – An exclusive lithological selection of possible martian earth analogues. Planetary and Space Science. ISSN 0032-0633. 208. doi: 10.1016/j.pss.2021.105339. Full text in Research Archive Show summary

  The Planetary Terrestrial Analogues Library (PTAL) is a dedicated lithological collection that currently consists of 102 terrestrial rock samples selected to be possible Mars analogues. The ultimate goal is improving future remote mineralogical and petrological analysis on Mars and other planetary bodies based on selected analysis such as Near- Infrared Reflectance Spectroscopy (NIR), Raman spectroscopy, Laser Induced Breakdown Spectroscopy (LIBS) and X-ray diffraction (XRD). Most international standards applied in the remote martian mineralogical and petrological analysis have so far been based on single, pure mineral analysis, with minimal interferences from other naturally occurring minerals. Here we present detailed lithological sample evaluations based on field appearance along with optical and XRD analysis of key terrestrial rock types. The detailed mineralogical and petrological descriptions give good basis for more complete lithological understanding. In combination with NIR, LIBS and Raman analysis of the very same samples PTAL aims at improving mineralogical and petrographical information from future rovers on Mars e.g. NASA's Mars2020-Perseverance and ESA and Roscosmos's ExoMars - Rosalind Franklin. The PTAL sample collection covers exclusively collected volcanic, magmatic and various sedimentary rocks and regoliths from well-known locations all over the world. These samples have a general composition comparable to what is currently known from Mars. The strength of this sample collection is its origin as common whole rock samples, in which minerals occur in their natural settings. It thereby allows studying possible detection interferences and a comparison of the sensitivity of the different techniques. The collection, in addition, forms the base for various alteration studies to better understand and explain alteration and weathering conditions on Mars. The complete results and sample preparations will be available to all scientists interested.

• Krzesinska, Agata Magdalena; Bultel, Benjamin Gabriel Rene; Loizeau, Damien; Craw, David; April, Richard & Poulet, Francois [Show all 7 contributors for this article] (2021). Mineralogical and spectral (NIR) characterization of Fe-rich vermiculite-bearing terrestrial deposits and constraints for mineralogy of Oxia Planum, ExoMars 2022 landing site. Astrobiology. ISSN 1531-1074. 21(8), p. 997–1016. doi: 10.1089/ast.2020.2410. Full text in Research Archive Show summary

  Oxia Planum is a Noachian plain on Mars. It was chosen as the final landing site for in situ studies by ExoMars 2022 rover. The main scientific objectives of the mission are to understand the mineralogy and aqueous evolution of ancient Mars with relevance to habitability. Oxia is covered by vast deposits of Fe,Mg-phyllosilicates, but the exact nature of these deposits is not yet fully understood. We performed a survey of potential terrestrial analog rocks, and here we show combined mineralogical characterization of these rocks with their near-infrared spectral analysis. Samples from two terrestrial sites were studied: (1) vermiculitized chlorite-schists from Otago, New Zealand, which underwent an alteration process without significant oxidation; and (2) basaltic tuffs from Granby, Massachusetts, USA, with Fe-rich clays filling amygdales of supposedly hydrothermal origin. Both analogues are incorporated into the newly built Planetary Terrestrial Analogue Library (PTAL) collection. Oxia bedrock clay-rich deposits are spectrally matched best by a well-crystallized trioctahedral vermiculite/saponite mixture from the basaltic tuff, although the contribution of saponite must be minor. Otago vermiculite is a good analogue to Oxia vermiculite in terms of overall mineralogy and Fe content. However, spectral inconsistencies related to the Al content in the Otago clays indicate that illitization of vermiculite, which results from postalteration oxidation, did not occur at Oxia. This implies limited water/rock interactions and reducing conditions during deposition of sediments now constituting the bedrock at Oxia. Whereas the spectral match does not conclusively imply the mineralogy, trioctahedral vermiculite should be considered a likely mineral component of the bedrock unit at Oxia Planum. Vermiculite has great potential to store organic matter, and the postdeposition geological context of Oxia Planum derived from understanding of environmental conditions in analog sites is promising for organic matter preservation.

• Lantz, Cateline; Poulet, Francois; Loizeau, Damien; Riu, Lucie; Pilorget, C. & Carter, John [Show all 9 contributors for this article] (2020). Planetary Terrestrial Analogues Library project: 1. characterization of samples by near-infrared point spectrometer. Planetary and Space Science. ISSN 0032-0633. 189. doi: 10.1016/j.pss.2020.104989. Full text in Research Archive Show summary

  The PTAL project aims at building and exploiting a database involving several analytical techniques, the Planetary Terrestrial Analogues Library, to help characterizing the mineralogical evolution of terrestrial bodies, starting with Mars. A total of 94 natural Earth rocks have been collected from selected locations around the world to get a selection of analogues for Martian geology. The PTAL library gathers a variety of igneous rocks from different plutonic and volcanic origins and compositions, associated to different environments and levels of aqueous alteration. Samples of impact craters and sedimentary units are also present. The full set of samples will be characterized with optical thin section analysis and XRD (Oslo University, Norway), NIR spectroscopy (Paris-Saclay University, France), Raman spectroscopy (Valladolid University, Spain) and LIBS (Paul Sabatier University, France). The multianalytical study used within the PTAL project provides an unique opportunity to coordinate minerals/elements detection by different techniques that are similar to the instruments onboard current and forthcoming Martian missions. Such combined analysis should give the opportunity to prepare and improve ExoMars/ESA-Roscosmos and Mars2020/NASA observations. This paper focuses only on the NIR measurements and interpretations. The diversity of the PTAL samples is well revealed by the diversity of spectra from the NIR observations. The detected minerals are representative of various formation, alteration and geochemical environments. The major diagnostic features observed are those of primary Fe2+ bearing silicates like olivine or pyroxene with low and/or high calcium content; altered silicates detected with vibrational features associated to OH and/or H2O and/or metal-OH features; oxides; zeolites; and carbonates. This collection brings together a set of rocks and minerals that have been reported elsewhere in the Solar System and particularly on Mars.

• Karlsson, Rebecca Vilde Martine Krohn; Cheng, Kar Wei; Crameri, Fabio; Rolf, Tobias; Uppalapati, Sruthi & Werner, Stephanie (2020). Implications of Anomalous Crustal Provinces for Venus' Resurfacing History. Journal of Geophysical Research (JGR): Planets. ISSN 2169-9097. 125(10). doi: 10.1029/2019JE006340. Full text in Research Archive
• Brasser, Ramon; Werner, Stephanie & Mojzsis, Stephen J. (2020). Impact bombardment chronology of the terrestrial planets from 4.5 Ga to 3.5 Ga. Icarus (New York, N.Y. 1962). ISSN 0019-1035. 338. doi: 10.1016/j.icarus.2019.113514. Full text in Research Archive
• Veneranda, Marco; Lopez-Reyes, Guillermo; Manrique, Jose Antonio; Medina, Jesus; Ruiz-Galende, Patricia & Torre-Fdez, Imanol [Show all 12 contributors for this article] (2020). ExoMars raman laser spectrometer: A tool for the potential recognition of wet-target craters on mars. Astrobiology. ISSN 1531-1074. 20(3), p. 349–363. doi: 10.1089/ast.2019.2095. Full text in Research Archive
• Uppalapati, Sruthi; Rolf, Tobias; Crameri, Fabio & Werner, Stephanie (2020). Dynamics of Lithospheric Overturns and Implications for Venus's Surface. Journal of Geophysical Research (JGR): Planets. ISSN 2169-9097. 125(11). doi: 10.1029/2019JE006258. Full text in Research Archive
• Loizeau, Damien; Lequertier, Guillaume; Poulet, Francois; Hamm, Vincent; Pilorget, Cédric & Meslier-Lourit, Lionel [Show all 10 contributors for this article] (2020). Planetary Terrestrial Analogues Library project: 2. building a laboratory facility for MicrOmega characterization. Planetary and Space Science. ISSN 0032-0633. 193. doi: 10.1016/j.pss.2020.105087. Full text in Research Archive Show summary

  Multiple spectroscopic techniques have been selected on previous, present and forthcoming missions to explore planetary surfaces in the Solar System. In particular, forthcoming ESA/Roscosmos and NASA missions to the surface of Mars will bring instruments capable of near-infrared (NIR), Raman and Laser Induced Breakdown Spectroscopies to analyze the mineralogy and chemistry of rocks. The PTAL (Planetary Terrestrial Analogues Library) project aims at building a multi-instrument spectral database of a large variety of natural Earth rock samples, including Mars analogues. The NIR hyperspectral microscope MicrOmega was selected to characterize the mineralogy of these analogues within the PTAL project. The instrument model used for the PTAL project is a spare flight model that requires specific care. For the safety of the instrument, and because of the large number of samples in the PTAL library and the requirement to optimize the observational conditions, a dedicated and semi-automated setup was built for the use of the MicrOmega instrument for this project. This paper presents the requirements specified for this setup, the technical solutions that have been selected, their implementation and the performances of the set-up. Sample preparation and operations during sample observations are explained, and a characterization example is presented to briefly illustrate the capabilities of MicrOmega in this set-up. The complete results from the MicrOmega characterizations of the PTAL rock analogues will be presented in a forthcoming paper (Loizeau et al. in prep).

• Wong, Emily W.; Brasser, R. & Werner, Stephanie C. (2020). Early impact chronology of the icy regular satellites of the outer solar system. Icarus (New York, N.Y. 1962). ISSN 0019-1035. 358. doi: 10.1016/j.icarus.2020.114184. Full text in Research Archive
• Sætre, Christian; Hellevang, Helge; Riu, Lucie; Dypvik, Henning; Pilorget, C & Poulet, Francois [Show all 7 contributors for this article] (2019). Experimental hydrothermal alteration of basaltic glass with relevance to Mars. Meteoritics and Planetary Science. ISSN 1086-9379. 54(2), p. 357–378. doi: 10.1111/maps.13214. Full text in Research Archive Show summary

  Phyllosilicates, carbonates, zeolites, and sulfates on Mars give clues about the planet's past environmental conditions, but little is known about the specific conditions in which these minerals formed within the crust and at the surface. The aim of the present study was to gain increased understanding on the formation of secondary phases by hydrothermal alteration of basaltic glass. The reaction processes were studied under varying conditions (temperature, pCO2, water:rock ratio, and fluid composition) with relevance to aqueous hydrothermal alteration in fully and partly saturated Martian basalt deposits. Analyses made on reaction products using X-ray diffraction (XRD) and scanning electron microscope (SEM) were compared with near infrared spectroscopy (NIR) to establish relative detectability and spectral signatures. This study demonstrates that comparable alteration minerals (phyllosilicates, carbonates, zeolites) form from vapor condensing on mineral surfaces in unsaturated sediments and not only in fully water-saturated sediments. In certain environments where water vapor might be present, it can alter the basaltic bedrock to a suite of authigenic phases similar to those observed on the Martian surface. For the detection of the secondary phases, XRD and SEM-EDS were found to be superior to NIR for detecting and characterizing zeolites. The discrepancy in detectability of zeolites between NIR and XRD/SEM-EDS might indicate that zeolites on Mars are more abundant than previously thought.

• Viennet, Jean-Christophe; Bultel, Benjamin & Werner, Stephanie C. (2019). Experimental reproduction of the martian weathering profiles argues for a dense Noachian CO2 atmosphere. Chemical Geology. ISSN 0009-2541. 525, p. 82–95. doi: 10.1016/j.chemgeo.2019.07.009. Full text in Research Archive
• Wu, Bo; Wang, Yiran; Lin, Tao Jun; Hu, Han & Werner, Stephanie C. (2019). Impact cratering in and around the Orientale Basin: Results from recent high-resolution remote sensing datasets. Icarus (New York, N.Y. 1962). ISSN 0019-1035. 333, p. 343–355. doi: 10.1016/j.icarus.2019.06.018. Full text in Research Archive
• Werner, Stephanie C. (2019). In situ calibration of the Martian cratering chronology. Meteoritics and Planetary Science. ISSN 1086-9379. 54(5), p. 1182–1193. doi: 10.1111/maps.13263. Full text in Research Archive
• Veneranda, Marco; Manrique-Martinez, Jose Antonio; Lopez-Reyes, Guillermo; Medina, Jesus E.; Torre-Fdez, Imanol & Castro, Kepa [Show all 13 contributors for this article] (2019). Spectroscopic study of olivine-bearing rocks and its relevance to the ExoMars rover mission. Spectrochimica Acta Part A - Molecular and Biomolecular Spectroscopy. ISSN 1386-1425. 223. doi: 10.1016/j.saa.2019.117360. Full text in Research Archive
• Mojzsis, Stephen J; Brasser, Ramon; Kelly, Nigel M.; Abramov, Oleg & Werner, Stephanie C. (2019). Onset of Giant Planet Migration before 4480 Million Years Ago. The Astrophysical Journal (ApJ). ISSN 0004-637X. 881(1). doi: 10.3847/1538-4357/ab2c03. Full text in Research Archive Show summary

  Soon after their formation, the terrestrial planets experienced intense impact bombardment by comets, leftover planetesimals from primary accretion, and asteroids. This temporal interval in solar system evolution, termed late accretion, thermally and chemically modified solid planetary surfaces and may have impeded life's emergence on the Hadean (pre-3850 Ma) Earth. The sources and tempo of bombardment, however, remain obscure. Here we present a timeline that relates variably retentive radiometric ages documented from asteroidal meteorites to new dynamical models that invoke an early episode of planetesimal-driven giant planet migration after the dispersal of the protoplanetary disk. Reconciliation of geochronological data with dynamical models shows that such giant planet migration should lead to an intense ~30 Myr influx of comets to the entire solar system manifested in radiometric age data. The absence of wholesale crustal reset ages after ~4450 Ma for the most resilient chronometers from Earth, Moon, Mars, 4 Vesta, and various meteorite parent bodies confines the onset of giant planet migration to ca. 4480 Ma. Waning impacts continue to strike the inner planets through a protracted monotonic decline in impactor flux, in agreement with predictions from crater chronology. New global 3D thermal analytical bombardment models derived from our revised impact mass-production functions show also that persistent niches for prebiotic chemistry leading to the emergence of life on the early Hadean Earth could endure late accretion since at least about 4400 million years ago.

• Wong, EW; Brasser, R. & Werner, Stephanie C. (2019). Impact bombardment on the regular satellites of Jupiter and Uranus during an episode of giant planet migration. Earth and Planetary Science Letters. ISSN 0012-821X. 506, p. 407–416. doi: 10.1016/j.epsl.2018.11.023. Full text in Research Archive
• Veneranda, Marco; Saiz, Jesus; Sanz-Arranz, Aurelio; Manrique, Jose Antonio; Lopez-Reyes, Guillermo & Medina, Jesus [Show all 9 contributors for this article] (2019). Planetary Terrestrial Analogues Library (PTAL) project: Raman data overview. Journal of Raman Spectroscopy. ISSN 0377-0486. doi: 10.1002/jrs.5652. Full text in Research Archive
• Bultel, Benjamin; Viennet, Jean-Christophe; Poulet, Francois; Carter, John & Werner, Stephanie C. (2019). Detection of Carbonates in Martian Weathering Profiles. Journal of Geophysical Research (JGR): Space Physics. ISSN 2169-9380. 124(4), p. 989–1007. doi: 10.1029/2018JE005845. Full text in Research Archive Show summary

  Noachian surfaces on Mars exhibit vertical assemblages of weathering horizons termed as weathering profiles; this indicates that surface water caused alteration of the rocks that required a different, warmer climate than today. Evidence of this early Martian climate with CO2 vapor as the main component causing greenhouse warming has been challenged by the lack of carbonate in these profiles. Here we report the analysis of Compact Reconnaissance Imaging Spectrometer for Mars L‐detector data leading to the detections of carbonates using a spectral signature exclusively attributed to them. The carbonates are collocated with hydroxylated minerals in weathering profiles over the Martian surface. The origin of CO2 for the formation of carbonates could be the atmosphere. The widespread distribution of weathering profiles with carbonates over the surface of the planet suggest global interactions between fluids containing carbonate/bicarbonate ions with the surface of Mars in the presence of atmospheric water until around 3.7 billion years ago. ©2019. American Geophysical Union. All Rights Reserved.

• Prieur, Nils Charles; Rolf, Tobias; Wünnemann, Kai & Werner, Stephanie C. (2018). Formation of simple impact craters in layered targets: Implications for lunar crater morphology and regolith thickness. Journal of Geophysical Research (JGR): Planets. ISSN 2169-9097. 123(6), p. 1555–1578. doi: 10.1029/2017JE005463. Full text in Research Archive Show summary

  Impact crater morphologies vary significantly across the lunar maria. Craters with diameter less than 400 m are closely related to variations in target properties (rock strength, porosity, and layering) as well as the impact velocity. Here we investigate target and impact conditions feasible for reproducing crater morphologies, such as normal, central‐mound, flat‐bottomed, and concentric craters, using numerical models of impact crater formation in two‐layer targets under lunar conditions (i.e., average‐impact velocity and gravity). Based on more than 1,000 numerical models, we observe that concentric craters can form with a strength contrast as low as factor of 2 between the layers as long as the difference in cohesion is larger than a value between 50 and 450 kPa (for an impact velocity of 12.7 km/s). Because of this small contrast, concentric craters do not serve as a good indication for the lunar regolith‐mare interface. Crater morphology changes with crater diameter according to three different scenarios depending on layers' strengths and the impact velocity. For high‐impact velocity or/and moderate material strength, normal crater morphology transitions directly to concentric morphology, while with large material strengths and/or low‐impact velocity, craters change with size from normal to flat‐bottomed and then to concentric morphology; only this latter pathway is consistent with previous laboratory results. Lunar regolith thicknesses estimated from crater morphologies can differ by up to 80% from previously inferred thicknesses. The transition from normal to flat‐bottomed craters is found to be the most robust transition to infer the thickness of the surficial target layer.

• Tinetti, Giovanna; Drossart, Pierre; Eccleston, Paul; Hartogh, Paul; Heske, Astrid & Leconte, Jérémy [Show all 244 contributors for this article] (2018). A chemical survey of exoplanets with ARIEL. Experimental astronomy (Print). ISSN 0922-6435. 46(1), p. 135–209. doi: 10.1007/s10686-018-9598-x. Full text in Research Archive
• Rolf, Tobias; Steinberger, Bernhard; Uppalapati, Sruthi & Werner, Stephanie C. (2018). Inferences on the mantle viscosity structure and the post-overturn evolutionary state of Venus. Icarus (New York, N.Y. 1962). ISSN 0019-1035. 313, p. 107–123. doi: 10.1016/j.icarus.2018.05.014. Full text in Research Archive
• Sekhar, Aswin; Asher, D.J.; Werner, Stephanie C.; Vaubaillon, J. & Li, G. (2017). Change in General Relativistic Precession Rates due to Lidov-Kozai oscillations in the Solar System. Monthly notices of the Royal Astronomical Society. ISSN 0035-8711. 468(2), p. 1405–1404. doi: 10.1093/mnras/stx548. Full text in Research Archive Show summary

  Both general relativistic (GR) precession and the Lidov–Kozai mechanism, separately, are known to play an important role in the orbital evolution of Solar system bodies. Previous works have studied these two mechanisms independently in great detail. However, both these phenomena occurring at the same time in real Solar system bodies have rarely been explored. In this work, we find a continuum connecting the GR precession dominant and Lidov–Kozai-like mechanism dominant regimes, i.e. an intermediate regime where the competing effects of GR precession and Lidov–Kozai-like oscillations coexist simultaneously. We find some real examples in the Solar system in this intermediate regime. Moreover, we identify a rare example among them, comet 96P/Machholz 1, which shows significant changes in the rates of GR precession (an order of magnitude higher than Mercury's GR precession rate) due to sungrazing and sun-colliding phases induced by Lidov–Kozai-like oscillations. This comet's combination of orbital elements and initial conditions (at the present epoch) favour this measurable rapid change in GR precession (at some points peaking up to 60 times Mercury's GR precession rate) along with prograde–retrograde inclination flip (due to Lidov–Kozai-like oscillations). Similar tests are performed for hundreds of bodies lying in the moderately low perihelion distance and moderately low semimajor axis phase space in the Solar system, the present lowest perihelion distance asteroid 322P/SOHO 1, and further examples connected with 96P/Machholz 1 namely, the Marsden and Kracht families of sungrazing comets plus low perihelion meteoroid streams like Daytime Arietids and Southern Delta Aquariids. © 2017 Oxford University Press

• Rolf, Tobias; Zhu, Meng-Hua; Wünnemann, Kai & Werner, Stephanie C. (2017). The role of impact bombardment history in lunar evolution. Icarus (New York, N.Y. 1962). ISSN 0019-1035. 286, p. 138–152. doi: 10.1016/j.icarus.2016.10.007. Full text in Research Archive
• Prieur, Nils Charles; Rolf, Tobias; Luther, Robert; Wunnemann, Kai; Xiao, Zhiyong & Werner, Stephanie C. (2017). The effect of target properties on transient crater scaling for simple craters. Journal of Geophysical Research (JGR): Biogeosciences. ISSN 2169-8953. 122(8), p. 1704–1726. doi: 10.1002/2017JE005283. Full text in Research Archive Show summary

  The effects of the coefficient of friction and porosity on impact cratering are not sufficiently considered in scaling laws that predict the crater size from a known impactor size, velocity, and mass. We carried out a systematic numerical study employing more than 1000 two‐dimensional models of simple crater formation under lunar conditions in targets with varying properties. A simple numerical setup is used where targets are approximated as granular or brecciated materials, and any compression of porous materials results in permanent compaction. The results are found to be consistent with impact laboratory experiments for water, low‐strength and low‐porosity materials (e.g., wet sand), and sands. Using this assumption, we found that both the friction coefficient and porosity are important for estimating transient crater diameters as is the strength term in crater scaling laws, i.e., the effective strength. The effects of porosity and friction coefficient on impact cratering were parameterized and incorporated into π group scaling laws, and predict transient crater diameters within an accuracy of ±5% for targets with friction coefficients f ≥ 0.4 and porosities Φ = 0–30%. Moreover, 90 crater scaling relationships are made available and can be used to estimate transient crater diameters on various terrains and geological units with different coefficient of friction, porosity, and cohesion. The derived relationships are most robust for targets with Φ > 10–15%, applicable for a lunar environment, and could therefore yield significant insights into the influence of target properties on cratering statistics. © 2017 American Geophysical Union

• Vago, Jorge L.; Westall, Frances; Coates, Andrew J.; Jaumann, Ralf; Korablev, Oleg & Ciarletti, Valérie [Show all 68 contributors for this article] (2017). Habitability on early Mars and the search for biosignatures with the ExoMars Rover. Astrobiology. ISSN 1531-1074. 17(6-7), p. 471–510. doi: 10.1089/ast.2016.1533. Full text in Research Archive
• Viennet, Jean-Christophe; Bultel, Benjamin; Riu, Lucie & Werner, Stephanie C. (2017). Dioctahedral Phyllosilicates Versus Zeolites and Carbonates Versus Zeolites Competitions as Constraints to Understanding Early Mars Alteration Conditions. Journal of Geophysical Research (JGR): Planets. ISSN 2169-9097. 122(11), p. 2328–2343. doi: 10.1002/2017JE005343. Full text in Research Archive
• Ashwal, Lewis; Torsvik, Trond Helge; Horvath, P.; Harris, C; Webb, S. & Werner, Stephanie C. [Show all 7 contributors for this article] (2016). A Mantle-derived Origin for Mauritian Trachytes. Journal of Petrology. ISSN 0022-3530. 57(9), p. 1645–1675. doi: 10.1093/petrology/egw052. Full text in Research Archive
• Brasser, R.; Matsumura, S.; Ida, S.; Mojzsis, S. J. & Werner, Stephanie C. (2016). ANALYSIS of TERRESTRIAL PLANET FORMATION by the GRAND TACK MODEL: SYSTEM ARCHITECTURE and TACK LOCATION. The Astrophysical Journal (ApJ). ISSN 0004-637X. 821(2). doi: 10.3847/0004-637X/821/2/75. Full text in Research Archive
• Ehlmann, Bethany L.; Anderson, F. Scott; Andrews-Hanna, Jeffrey C.; Catling, David C.; Christensen, Philip R. & Cohen, Barbara Anne [Show all 46 contributors for this article] (2016). The sustainability of habitability on terrestrial planets: Insights, questions, and needed measurements from Mars for understanding the evolution of Earth-like worlds. Journal of Geophysical Research (JGR): Biogeosciences. ISSN 2169-8953. 121(10), p. 1927–1961. doi: 10.1002/2016JE005134. Full text in Research Archive
• Xiao, Zhiyong; Prieur, Nils Charles & Werner, Stephanie C. (2016). The self-secondary crater population of the Hokusai crater on Mercury. Geophysical Research Letters. ISSN 0094-8276. 43(14), p. 7424–7432. doi: 10.1002/2016GL069868. Full text in Research Archive Show summary

  Whether or not self‐secondaries dominate small crater populations on continuous ejecta deposits and floors of fresh impact craters has long been a controversy. This issue potentially affects the age determination technique using crater statistics. Here the self‐secondary crater population on the continuous ejecta deposits of the Hokusai crater on Mercury is unambiguously recognized. Superposition relationships show that this population was emplaced after both the ballistic sedimentation of excavation flows and the subsequent veneering of impact melt, but it predated the settlement and solidification of melt pools on the crater floor. Fragments that formed self‐secondaries were launched via impact spallation with large angles. Complex craters on the Moon, Mercury, and Mars probably all have formed self‐secondaries populations. Dating young craters using crater statistics on their continuous ejecta deposits can be misleading. Impact melt pools are less affected by self‐secondaries. Overprint by subsequent crater populations with time reduces the predominance of self‐secondaries. © 2016 American Geophysical Union

• Brasser, R.; Mojzsis, S. J.; Werner, Stephanie C.; Matsumura, S. & Ida, S. (2016). Late veneer and late accretion to the terrestrial planets. Earth and Planetary Science Letters. ISSN 0012-821X. 455, p. 85–93. doi: 10.1016/j.epsl.2016.09.013. Full text in Research Archive
• Schmieder, Martin; Schwarz, Winfried H.; Trieloff, M.; Buchner, Elmar; Hopp, Jens & Tohver, Eric [Show all 11 contributors for this article] (2016). The two Suvasvesi impact structures, Finland: Argon isotopic evidence for a "false" impact crater doublet. Meteoritics and Planetary Science. ISSN 1086-9379. 51(5), p. 966–980. doi: 10.1111/maps.12636. Full text in Research Archive
• Quantin, Cathy; Popova, Olga; Hartmann, William K & Werner, Stephanie C. (2016). Young Martian crater Gratteri and its secondary craters. Journal of Geophysical Research (JGR): Planets. ISSN 2169-9097. 121(7), p. 1118–1140. doi: 10.1002/2015JE004864. Full text in Research Archive
• Xiao, Zhiyong & Werner, Stephanie C. (2015). Size-frequency distribution of crater populations in equilibrium on the Moon. Journal of Geophysical Research (JGR): Biogeosciences. ISSN 2169-8953. 120(12), p. 2277–2292. doi: 10.1002/2015JE004860. Full text in Research Archive
• Torsvik, Trond Helge; Amundsen, Hans E. Foss; Trønnes, Reidar G; Doubrovine, Pavel; Gaina, Carmen & Kusznir, Nick J. [Show all 12 contributors for this article] (2015). Continental crust beneath southeast Iceland. Proceedings of the National Academy of Sciences of the United States of America (PNAS). ISSN 0027-8424. 112(15), p. E1818–E1827. doi: 10.1073/pnas.1423099112. Full text in Research Archive Show summary

  The magmatic activity (0–16 Ma) in Iceland is linked to a deep mantle plume that has been active for the past 62 My. Icelandic and northeast Atlantic basalts contain variable proportions of two enriched components, interpreted as recycled oceanic crust supplied by the plume, and subcontinental lithospheric mantle derived from the nearby continental margins. A restricted area in southeast Iceland—and especially the Öræfajökull volcano—is characterized by a unique enriched-mantle component (EM2-like) with elevated 87Sr/86Sr and 207Pb/204Pb. Here, we demonstrate through modeling of Sr–Nd–Pb abundances and isotope ratios that the primitive Öræfajökull melts could have assimilated 2–6% of underlying continental crust before differentiating to more evolved melts. From inversion of gravity anomaly data (crustal thickness), analysis of regional magnetic data, and plate reconstructions, we propose that continental crust beneath southeast Iceland is part of ∼350-km-long and 70-km-wide extension of the Jan Mayen Microcontinent (JMM). The extended JMM was marginal to East Greenland but detached in the Early Eocene (between 52 and 47 Mya); by the Oligocene (27 Mya), all parts of the JMM permanently became part of the Eurasian plate following a westward ridge jump in the direction of the Iceland plume.

• Steinberger, Bernhard; Zhao, Dapeng & Werner, Stephanie C. (2015). Interior structure of the Moon: Constraints from seismic tomography, gravity and topography. Physics of the Earth and Planetary Interiors. ISSN 0031-9201. 245, p. 26–39. doi: 10.1016/j.pepi.2015.05.005. Full text in Research Archive Show summary

  Seismic tomography can be combined with constraints from geoid, topography and other surface observations to gain information about mantle structure and dynamics. This approach has been taken with much success for the Earth mantle, and here it is, for the first time, applied to the Moon. Lunar tomography has much lower resolution as for the Earth and is mostly restricted to the near side, nevertheless we can assess under what assumptions the fit between predicted geoid (based on a tomography model) and observed geoid is best. Among the models tested, we find the most similar pattern (correlation about 0.5) if we only consider tomography below 225 km depth, if density anomalies cause little or no dynamic topography and if we compare to the geoid with the flattening (l=2,m=0l=2,m=0) term removed. This could mean that (a) like for the Earth, seismic anomalies shallower than 225 km are caused by a combination of thermal and compositional effects and therefore cannot be simply converted to density anomalies; (b) the lithosphere is sufficiently thick to prevent dynamic topography more than a small fraction of total topography; and (c) flattening is a “fossil” bulge unrelated to present-day mantle anomalies. However, we have to be cautious with interpreting our results, because for models with a comparatively higher correlation and a conversion from seismic velocity to density anomalies similar to the Earth’s upper mantle, the amplitude of the predicted geoid is much lower than observed. This could either mean that the tomography model is strongly damped, or that the geoid is mostly due to shallow causes such as crustal thickness variations, with only a small part coming from the deeper mantle.

• Werner, Stephanie C. (2014). Moon, Mars, Mercury: Basin formation ages and implications for the maximum surface age and the migration of gaseous planets. Earth and Planetary Science Letters. ISSN 0012-821X. 400, p. 54–65. doi: 10.1016/j.epsl.2014.05.019. Full text in Research Archive
• Rauer, Heike; Catala, C; Aerts, C; Appourchaux, T; Benz, W & Brandeker, A [Show all 160 contributors for this article] (2014). The PLATO 2.0 mission. Experimental astronomy (Print). ISSN 0922-6435. 38(1-2), p. 249–330. doi: 10.1007/s10686-014-9383-4. Full text in Research Archive
• Werner, Stephanie C.; Ody, Anouck & Poulet, Francois (2014). The source crater of martian shergottite meteorites. Science. ISSN 0036-8075. 343(6177), p. 1343–1346. doi: 10.1126/science.1247282. Full text in Research Archive
• Fritz, Jörg N.; Bitsch, Bertram; Kuhrt, Ekkehard K.; Morbidelli, Alessandro; Tornow, Carmen & Wunnemann, Kai [Show all 11 contributors for this article] (2014). Earth-like habitats in planetary systems. Planetary and Space Science. ISSN 0032-0633. 98, p. 254–267. doi: 10.1016/j.pss.2014.03.003. Full text in Research Archive
• Owen-Smith, T.M.; Ashwal, L.D.; Torsvik, Trond Helge; Ganerød, Morgan; Nebel, O & Webb, S. J. [Show all 7 contributors for this article] (2013). Seychelles alkaline suite records the culmination of Deccan Traps continental flood volcanism. Lithos. ISSN 0024-4937. 182-183, p. 33–47. doi: 10.1016/j.lithos2013.09.011. Full text in Research Archive
• Gaina, Carmen; Medvedev, Sergei; Torsvik, Trond Helge; Koulakov, I.Yu & Werner, Stephanie C. (2013). 4D Arctic: A Glimpse into the Structure and Evolution of the Arctic in the Light of New Geophysical Maps, Plate Tectonics and Tomographic Models. Surveys in geophysics. ISSN 0169-3298. 35, p. 1095–1122. doi: 10.1007/s10712-013-9254-y. Full text in Research Archive
• Gaina, Carmen; Torsvik, Trond Helge; Hinsbergen, Douwe Van; Medvedev, Sergei; Werner, Stephanie C. & Labails, C (2013). The African Plate: A history of oceanic crust accretion and subduction since the Jurassic. Tectonophysics. ISSN 0040-1951. 604, p. 4–25. doi: 10.1016/j.tecto.2013.05.037. Full text in Research Archive
• Burke, Kevin; Werner, Stephanie; Steinberger, Bernard & Torsvik, Trond Helge (2012). Why is the areoid like the residual geoid? Geophysical Research Letters. ISSN 0094-8276. 39(17). doi: 10.1029/2012GL052701. Full text in Research Archive Show summary

  The equipotential figures of Earth (residual geoid), and of Mars (areoid) are characterized by pairs of elevated and pairs of depressed antipodal equatorial regions. Elevated regions of the residual geoid lie vertically above the two Large Low Shear Wave Velocity Provinces (LLSVPs) on the Core Mantle Boundary (CMB). There is evidence that the LLSVPs are dense, physicochemically distinct, and have been stable in their positions with respect to each other and to the Earth's spin axis for at least ∼550 My. The final event in the planetary‐scale development of the Earth's structure was the moon‐forming event and the comparable event on Mars is thought by many to have been the Borealis basin‐forming impact. We attribute the formation of the LLSVPs and postulated comparable masses underlying the elevated regions of the areoid on the CMB of Mars, to the immediate after‐effects of those two giant impacts. © 2012 American Geophysical Union

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• Bultel, Benjamin Gabriel Rene; Krzesinska, Agata Magdalena; Loizeau, Damien; Veneranda, Marco & Werner, Stephanie C. (2025). Deciphering the alteration processes by micro-scale characterization of vermiculite-rich sample from Granby Tuff, an analogue to Noachian clay deposits at Oxia Planum. doi: 10.5194/epsc-dps2025-1550. Full text in Research Archive
• Tjoflot, Gunn Kristin & Werner, Stephanie C. (2025). GEO-professor tildelt 12 millioner til forskning på eksoplaneter. [Internet]. titan.uio.no. doi: https:/www.titan.uio.no/universet/2025/geo-professor-tildelt-12mill-til-forskning-pa-eksoplaneter.html. Full text in Research Archive Show summary

  – Et mål med prosjektet er å få mer kunnskap om dannelsen av eksoplaneter, sier professor Stephanie Werner.

• Kohfeldt, Anja; Wahlén, Rebecka; Holdcroft, Sam; Teodoro, Luis Filipe Alves & Werner, Stephanie C. (2025). Element abundance mapping with the SER3NE Gamma-ray and neutron spectrometer. doi: 10.5194/epsc-dps2025-1439. Full text in Research Archive Show summary

  Selene’s Explorer for Roughness, Regolith, Resources, Neutrons and Elements (SER3NE) is a proposed small satellite mission in lunar orbit, aiming to characterize the lunar surface to unravel its volatile origin and delivery processes, in addition to uncovering the geological processes that shaped the Moon. Global element abundance mapping will prospect lunar resources for ISRU at future landing sites. Further, the mission is aiming to determine a more precise space-based neutron lifetime and the orbital evolution of the Earth-Moon system. To achieve these goals, SER3NE will host three instruments: a gamma-ray and neutron spectrometer (GRiNS, by UiO), the Lunar Infrared Point spectrometer (LIPS, by ROB/BIRA-IASB), and the SER3NE Laser Altimeter (S3LA, by DLR).Here, we present the current Gamma-Ray-including-Neutrons Spectrometer (GRiNS) design, performance specifications and preliminary results of the GRiNS laboratory demonstrator. GRiNS is part of the CLUNGAS family, that was reported on earlier.1By detecting gamma-ray and neutron radiation moderated by the lunar surface after GCR impact, GRiNS will be able to create global compositional maps and their abundances of different elements, such as Al, Ca, Fe, K, Mg, Si, Ti, Th, as well as hydrogen. In previous missions2 this was demonstrated with LaBr3 as main gamma-ray detector, proving the suitability of this technology. The default approach for hydrogen mapping are He3 pressurized tubes3, however, recently mission approaches with scintillator-based neutron detectors were launched4. In our approach we combine gamma-ray and neutron detection in one hybrid detector for reducing weight, cost, and space, and enabling deployment on small satellite missions.   GRiNS is a compact detector  capable of gamma-ray detection in the range of 100 keV to 8 MeV as well as the detection of thermal to epithermal neutrons. There shall be two detector units, facing nadir (for mapping) and zenith (in addition for neutron lifetime), as depicted in fig.1. The comparison of the ascending and descending gravitational bound thermal neutrons allow for the determination of the neutron lifetime along their flight path. The primary detecting material is a CLLBC (Cs2LiLa(Br,Cl)6:Ce), a dual-mode scintillator capable of both high-resolution gamma-ray spectroscopy and thermal to epi-thermal neutron detection. The preliminary detector layout aims for a 2x2 array where CLLBC is accompanied by lanthanum bromide (LaBr3), a crystal scintillator used in previous lunar mission2 for high-resolution gamma-ray spectroscopy, for improved gamma-ray – neutron discrimination. CLLBC and LaBr3 provide a good spectral resolution of

• Thorpe, M. T.; Velbel, M. A.; Hauber, E.; Tait, K. T.; Thiessen, F. & Sefton-Nash, E. [Show all 12 contributors for this article] (2025). The Mars Sample Return Analogue Sample Library. doi: https:/www.hou.usra.edu/meetings/lpsc2025/pdf/2109.pdf. Full text in Research Archive
• Werner, Stephanie (2025). Mars' historie. Astronomi. ISSN 0802-7587. Full text in Research Archive
• Boon, Annique van der & Werner, Stephanie (2024). Lonely exoPlanet – Din guide med anbefalinger for både populære og mindre kjente planeter. geoforskning.no. Full text in Research Archive
• Thiessen, F.; Krzesinska, A.M.; Orgel, C.; Sefton-Nash, E.; Hutzler, A. & Werner, Stephanie C. [Show all 9 contributors for this article] (2024). Mars sample return analogue sample library. Full text in Research Archive
• Shan, Yutong; Hatalova, Petra; Tabernero, Hugo; Timmermann, Anina; Mamonova, Elena & Werner, Stephanie C. (2024). Current limitations in chemical abundance measurements for M dwarfs and implications for exoplanet characterisation. Full text in Research Archive
• Shan, Yutong; Wedemeyer, Sven; Werner, Stephanie C. & Mamonova, Elena (2024). En leteaksjon av en annen verden: Kavliprisen i astrofysikk for 2024 hedrer forskerne som har pionert studien av eksoplaneter. Bladet Astronomi. Full text in Research Archive
• Harrington, Elise Michelle; Bultel, Benjamin; Krzesinska, Agata Magdalena & Werner, Stephanie C. (2020). Paleolakes and evaporite deposits across Mars. Full text in Research Archive
• Domeier, Mathew; Torsvik, Trond Helge; Conrad, Clinton Phillips; Steinberger, Bernhard; Doubrovine, Pavel & Trønnes, Reidar G [Show all 9 contributors for this article] (2019). On the stability of Earth’s degree 2 mantle structures. Full text in Research Archive
• Domeier, Mathew; Torsvik, Trond Helge; Conrad, Clinton Phillips; Steinberger, Bernhard; Doubrovine, Pavel V. & Trønnes, Reidar G [Show all 9 contributors for this article] (2019). On the stability of Earth’s degree 2 mantle structure. European Geosci. Union, Gen. Assembly, Geophys. Res. Abstr.. Full text in Research Archive
• Wong, Emily W.; Brasser, R. & Werner, Stephanie C. (2019). Corrigendum to “Impact bombardment on the regular satellites of Jupiter and Uranus during an episode of giant planet migration” (Earth and Planetary Science Letters (2019) 506 (407–416), (S0012821X18306824) (10.1016/j.epsl.2018.11.023)). Earth and Planetary Science Letters. ISSN 0012-821X. 508, p. 122–123. doi: 10.1016/j.epsl.2018.12.021. Full text in Research Archive
• Kulakov, Evgeniy; Doubrovine, Pavel V.; Torsvik, T.H; Werner, Stephanie C. & Silkoset, Petter (2018). Paleomagnetism of Late Jurassic – Early Cretaceous coast-parallel dykes in SW Greenland. Full text in Research Archive Show summary

  It is a well-known and still unresolved problem of the Jurassic to Early Cretaceous apparent polar wander paths (APWP) discrepancy between those for North America (Laurentia) and Eurasia. Paleomagnetic poles derived from coeval rocks from the two continents differ significantly with North American poles characterized by shallower pole latitudes. The APWP mismatch cannot be resolved by correction for inclination shallowing or using different plate circuits. One of the possible explanations for the observed phenomenon is that paleomagnetic data from North America show the effects of younger remagnetizations and/or tectonic rotation. In an attempt to resolve this problem, paleomagnetic study of samples from ~35 Late Jurassic to Early Cretaceous coast-parallel mafic dykes exposed in SW Greenland (part of Laurentia) was carried out. Paleomagnetic samples have been subjected to a step-wise thermal and alternating field demagnetization techniques which yielded well-defined characteristic remanent components. A primary nature of the characteristic remanence is supported by positive baked-contact tests and the presence of paleomagnetic directions of both polarities that pass a reversal test. Our results indicate that the paleomagnetic pole for Greenland has higher latitude than the coeval North American poles and plots closer to the APW path for Eurasia. We will discuss the results and their implications for global Mesozoic apparent polar wander and paleogeography during Jurassic and early Cretaceous times.

• Uppalapati, Sruthi; Rolf, Tobias; Crameri, Fabio; Conrad, Clinton Phillips & Werner, Stephanie C. (2018). How Venus’ young surface came to be: New insights from 2D and 3D modelling. Full text in Research Archive
• Uppalapati, Sruthi; Rolf, Tobias; Crameri, Fabio; Conrad, Clinton Phillips & Werner, Stephanie C. (2018). How Venus’ young surface came to be: New insights from 2D and 3D modelling. Full text in Research Archive
• Sekhar, Aswin; Asher, David; Werner, Stephanie C.; Vaubaillon, Jeremie & Li, Gongjie (2017). Rapid Enhancement in General Relativistic Precession Rates due to Lidov-Kozai oscillations. Full text in Research Archive
• Prieur, Nils Charles; Rolf, Tobias; Wünnemann, Kai & Werner, Stephanie C. (2017). Crater scaling results for final rim-to-rim crater diameter - Influence of angle of friction, cohesion and porosity on simple craters. Full text in Research Archive
• Sætre, Christian; Dypvik, Henning; Hellevang, Helge & Werner, Stephanie C. (2016). Earth Mars Analogues - Linking experimental and Martian clays. Full text in Research Archive
• Luther, Robert; Prieur, Nils Charles; Tasdelen, E; Wünnemann, Kai & Werner, Stephanie C. (2016). Shock melting, crater formation, and ejecta distribution in the 17th of March 2013 lunar impact event. Full text in Research Archive
• Prieur, Nils Charles; Luther, Robert; Rolf, Tobias; Wünnemann, Kai & Werner, Stephanie C. (2016). Target heterogeneities and their implications on crater scaling laws. Full text in Research Archive
• Xiao, Zhiyong; Prieur, Nils Charles & Werner, Stephanie C. (2016). Emplacement history of self-secondaries. Full text in Research Archive
• Prieur, Nils Charles; Xiao, Zhiyong; Wünnemann, Kai & Werner, Stephanie C. (2016). Effects of target properties on crater sizes and its implication on age determination - Insights from numerical experiments. Full text in Research Archive
• Werner, Stephanie C.; Prieur, Nils Charles; Sekhar, Aswin & Xiao, Zhiyong (2016). On the scaling of small impact craters on the Moon. Full text in Research Archive
• Prieur, Nils Charles; Luther, Robert; Wünnemann, Kai & Werner, Stephanie C. (2015). The effects of target properties on small-diameter crater size-frequency distribution - Numerical experiments. Full text in Research Archive
• Rolf, Tobias; Schott, Marc; Luther, Robert; Zhu, Meng-Hua; Wünnemann, Kai & Werner, Stephanie C. (2015). Thermal and volcanic evolution of small planetary bodies: Role of impact processes through ejecta deposits and shock heating. Full text in Research Archive
• Rolf, Tobias; Steinberger, Bernhard & Werner, Stephanie C. (2015). On the origin of Venus' unusual gravity spectrum. Full text in Research Archive
• Rolf, Tobias; Steinberger, Bernhard & Werner, Stephanie C. (2015). On the origin of Venus' unusual gravity spectrum. Full text in Research Archive
• Ashwal, Lewis; Torsvik, Trond Helge; Horvath, P.; Harris, C.; Webb, S. J. & Werner, Stephanie C. [Show all 7 contributors for this article] (2015). Evolved Rocks in Ocean Islands Formed by Melting of Metasomatized Mantle. Full text in Research Archive
• Werner, Stephanie C. (2013). Timing of the early bombardment history of Moon, Mars, and Mercury. Full text in Research Archive
• Galland, Olivier; Polteau, Stephane & Werner, Stephanie C. (2013). Coronae as a result of giant magma intrusions in the lithosphere of Venus: insights from laboratory experiments. Full text in Research Archive
• Steinberger, Bernhard & Werner, Stephanie C. (2013). Mantle dynamics models for Venus - comparison of spatial and spectral characteristics of inferred gravity anomalies and topography with observations. Full text in Research Archive
• Werner, Stephanie C.; Melosh, H.J.; McSween, H.Y.; Liu, Y.; Baziotis, I.P. & Bodnar, R.J. [Show all 8 contributors for this article] (2013). Mojave Crater: Possible Source for Martian Meteorites. Full text in Research Archive
• Werner, Stephanie C.; Ody, Anouck & Poulet, Francois (2013). Mojave Crater, Mars: One meteorite source crater. Full text in Research Archive

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