abstract: Impact cratering and volcanism are two fundamental processes that alter the surfaces of the terrestrial planets. Though well studied through laboratory experiments and terrestrial analogs, many questions remain regarding how these processes operate across the Solar System. Little is known about the formation of large impact basins (>300 km in diameter) and the degree to which they modify planetary surfaces. On the Moon, large impact basins dominate the terrain and are relatively well preserved. Because the lunar geologic timescale is largely derived from basin stratigraphic relations, it is crucial that we are able to identify and characterize materials emplaced as a result of the formation of the basins, such as light plains. Using high-resolution images under consistent illumination conditions and topography from the Lunar Reconnaissance Orbiter Camera (LROC), a new global map of light plains is presented at an unprecedented scale, revealing critical details of lunar stratigraphy and providing insight into the erosive power of large impacts. This work demonstrates that large basins significantly alter the lunar surface out to at least 4 radii from the rim, two times farther than previously thought. Further, the effect of pre-existing topography on the degradation of impact craters is unclear, despite their use in the age dating of surfaces. Crater measurements made over large regions of consistent coverage using LROC images and slopes derived from LROC topography show that pre-existing topography affects crater abundances and absolute model ages for craters up to at least 4 km in diameter. On Mars, small volcanic edifices can provide valuable insight into the evolution of the crust and interior, but a lack of superposed craters and heavy mantling by dust make them difficult to age date. On Earth, morphometry can be used to determine the ages of cinder cone volcanoes in the absence of dated samples. Comparisons of high-resolution topography from the Context Imager (CTX) and a two-dimensional nonlinear diffusion model show that the forms observed on Mars could have been created through Earth-like processes, and with future work, it may be possible to derive an age estimate for these features in the absence of superposed craters or samples. / Dissertation/Thesis / Doctoral Dissertation Geological Sciences 2018

The sources and sinks of energy for transient waves in the Martian atmosphere are investigated, applying diagnostic techniques developed for the analysis of terrestrial baroclinic waves to output from a Mars General Circulation Model. These diagnostic techniques include the vertically averaged eddy kinetic energy and regression analysis. The results suggest that the primary source of the kinetic energy of the waves is baroclinic energy conversion in localized regions. It is also shown that there exist preferred regions of baroclinic energy conversion. In addition, it is shown that downstream baroclinic development plays an important role in the evolution of the waves and in the baroclinic energy conversion process. This is the first time that evidence for downstream baroclinic development has been found for an atmosphere other than the terrestrial one.

The Alpha Particle X-ray Spectrometer (APXS) on the Mars Exploration Rovers possesses the ability to detect carbon and oxygen within martian samples via Rutherford backscattering principles. Several consecutive measurements of the martian atmosphere by Spirit, paralleled by Monte Carlo simulations, provided an energy calibration to mitigate the absence of an alpha-mode calibration pre-flight. Data from a pre-flight thermal acceptance test agreed with this energy calibration, confirming the presence of an unexpected offset. Correcting a bug in the APXS firmware resulted in a temperature-independent energy scale. A model was developed and applied to all atmospheric data illustrating a dip in atmospheric peak areas, potentially arising from a week-long weather event on Mars. An early expansion of this model to solid samples has not yet been able to detect any hydrated minerals or carbonates. Preliminary investigations into determining martian atmospheric pressure and potential elemental layering within samples shows promise.

abstract: Hydrogen isotope compositions of the martian atmosphere and crustal materials can provide unique insights into the hydrological and geological evolution of Mars. While the present-day deuterium-to-hydrogen ratio (D/H) of the Mars atmosphere is well constrained (~6 times that of terrestrial ocean water), that of its deep silicate interior (specifically, the mantle) is less so. In fact, the hydrogen isotope composition of the primordial martian mantle is of great interest since it has implications for the origin and abundance of water on that planet. Martian meteorites could provide key constraints in this regard, since they crystallized from melts originating from the martian mantle and contain phases that potentially record the evolution of the H2O content and isotopic composition of the interior of the planet over time. Examined here are the hydrogen isotopic compositions of Nominally Anhydrous Phases (NAPs) in eight martian meteorites (five shergottites and three nakhlites) using Secondary Ion Mass Spectrometry (SIMS). This study presents a total of 113 individual analyses of H2O contents and hydrogen isotopic compositions of NAPs in the shergottites Zagami, Los Angeles, QUE 94201, SaU 005, and Tissint, and the nakhlites Nakhla, Lafayette, and Yamato 000593. The hydrogen isotopic variation between and within meteorites may be due to one or more processes including: interaction with the martian atmosphere, magmatic degassing, subsolidus alteration (including shock), and/or terrestrial contamination. Taking into consideration the effects of these processes, the hydrogen isotope composition of the martian mantle may be similar to that of the Earth. Additionally, this study calculated upper limits on the H2O contents of the shergottite and nakhlite parent melts based on the measured minimum H2O abundances in their maskelynites and pyroxenes, respectively. These calculations, along with some petrogenetic assumptions based on previous studies, were subsequently used to infer the H2O contents of the mantle source reservoirs of the depleted shergottites (200-700 ppm) and the nakhlites (10-100 ppm). This suggests that mantle source of the nakhlites is systematically drier than that of the depleted shergottites, and the upper mantle of Mars may have preserved significant heterogeneity in its H2O content. Additionally, this range of H2O contents is not dissimilar to the range observed for the Earth’s upper mantle. / Dissertation/Thesis / Masters Thesis Geological Sciences 2015

abstract: The origin of the solar system and formation of planets such as Earth are among the most fascinating, outstanding scientific problems. From theoretical models to natural observations, it is possible to infer a general way of how the solar system evolved from the gravitational collapse of the molecular cloud to accretion and differentiation of planetary-sized bodies. This dissertation attempts to place additional constraints on the source, distribution, and evolution of chemical variability in the early solar system, Mars, and Earth. A new method was developed for the measurement of titanium isotopes in calcium-aluminum-rich inclusions (CAIs) by laser ablation multi-collector inductively coupled plasma mass spectrometry. The isotopic compositions of 17 Allende CAIs define a narrow range with clearly resolved excesses in 46Ti and 50Ti and suggests that "normal" CAIs formed from a relatively uniform reservoir. Petrologic and isotopic analysis of a new FUN (Fractionated and Unknown Nuclear effects) CAI suggests that normal and FUN CAIs condensed in similar environments, but subsequently evolved under vastly different conditions. Volatiles may have influenced the formation and evolution of basaltic magmas on Mars. Light lithophile element (LLE) and fluorine (F) concentrations and isotopic compositions of pyroxene determined in situ in several Martian meteorites suggests that the primary magmatic signature of LLE and F zonation in Shergottite pyroxene has been disturbed by post-crystallization diffusive equilibration. Using relevant crystal-melt partition coefficients the F contents for Martian meteorite parental melts are ~910 and ~220 ppm. Estimates of the F content in the Shergottite and Nakhlite source regions are similar to that of mid-ocean ridge basalts (MORB) and ocean island basalts (OIB), respectively, here on Earth. Noble gas systematics of OIBs relative to MORBs, suggests OIBs preferentially sample a primordial reservoir located within Earth's mantle. Geodynamic calculations were performed to investigate the time-dependent rate of material entrained into plumes from these primordial reservoirs. These models predict melts rising to the surface will contain variable proportions of primordial material. The results demonstrate that although high 3He/4He ratios may mandate a mantle plume that samples a primordial reservoir, more MORB-like 3He/4He ratios in OIBs do not preclude a deep plume source. / Dissertation/Thesis / Doctoral Dissertation Geological Sciences 2014

This thesis focuses on the long-term rotational stability of the Earth and terrestrial planets. One important class of perturbation is a reorientation of the solid planet with respect to a rotation pole that remains fixed in an inertial frame. These motions are driven by mass redistribution within or on the surface of the planet (e.g. glaciation, mantle convective flow). Long-term changes in the orientation of the rotation pole are called True Polar Wander (TPW). / Earth and Planetary Sciences

Iron (oxyhydr)oxide concretions in the Navajo Sandstone of southern Utah have been extensively researched as Martian analogues. However, the discovery of calcium carbonate concretions in areas such as Coyote Gulch, Utah, has encouraged recent studies to understand the relationship between calcium carbonate spheroidal concretions as possible precursors to iron (oxyhydr)oxide concretions, and to determine the fluid chemistries involved in diagenesis. This is important because nucleation and precipitation mechanisms of these spheroidal calcium carbonate and iron (oxyhydr)oxide concretions and fluid mechanisms in iron rich environments could affect the preservation of possible biosignatures in other subsurface features on Mars. The elemental and mineralogical compositions of the concretions were examined in order to determine physical and chemical features shared by the two types of concretions and did show that they share similar morphologies; however, the Coyote Gulch concretions are calcite cemented (~30 wt.%), with secondary iron (oxyhydr)oxide precipitation and decreases in calcite in transects away from the calcium carbonate concretions. Several chemical and mineralogical differences exist between the two separate populations of concretions, possibly due to regional variability of reacting phases in fluid systems. Spring fluids emanating from the Navajo Sandstone in Coyote Gulch were tested to determine the fluids responsible for the development of any of the concretion mineralogies in the study area which could form in distinctive geochemical systems. Geochemical modeling performed in this research explored the question of fluid chemistry involved in concretion formation in the Navajo Sandstone and findings suggest that the calcite concretions formed prior to the precipitation of secondary iron (oxyhydr)oxides and may have provided a localized buffering environment for the precipitation of iron (oxyhydr)oxides. Paleofluid circulation, redox processes, and elemental mobility are examined using the geochemistry of Navajo Sandstone concretions and host rock. Various simulations applicable to diagenetic fluids in the studied concretions show the importance of salinity and pH in paleoaquifers in order to precipitate mineral assemblages similar to those found in the Navajo Sandstone. Widespread dissolution features, major and trace element distributions, and geochemical modeling identified feasible fluid-rock interactions in paleofluids, including the importance of limited H2S gas and the limited feasibility of hydrocarbon rich fluids in concretion formation using current data. A universal mechanism for calcium carbonate to iron (oxyhydr)oxide concretion formation could be applied on other planets and provide exciting implications in the search for carbon rich redox gradients which could support life in the subsurface of otherwise inhospitable planets.

A few years ago, the charge-transfer reaction CO2+  +  O ⟶ O+ + CO2 was investigated experimentally for the first time since the study by Fehsenfeld et al., (1970). This new investigation was conducted by Tenewitz et al., (2018). The rate coefficient k < 6 × 10−13 cm3 s−1 , concluded by Tenewitz et al. (2018), differed substantially from the value of 9.6 × 10−11 cm3 s−1 reported by Fehsenfeld et al., (1970). Fox et al., (2021) showed that the old rate constants for the two channels of the CO2+  +  O interaction work much better than the new ones in reproducing chemical features of the Martian ionosphere. Here, we combine MAVEN/NGIMS and TIMED/SEE data to conduct model-observation comparisons of O+ concentrations in the dayside Martian ionosphere. We consider each orbit of the MAVEN Deep Dip 2 (DD2) campaign between 17-22 April 2015. In the model, we balance the production rate of O+ through the aforementioned charge transfer reaction and the photoionisation of O and CO2 , with the loss rate through the reaction O+ + CO2 ⟶ O2+ + CO. We find a better level of agreement between the modelled and the observed O+ concentrations— (i) towards closest approach altitudes (∼ 130 km), and (ii) when using the old rate constant instead of the new one for the charge transfer reaction CO2+ +  O ⟶ O+ + CO2 .

La modélisation physique en enceinte de gel est utilisée pour analyser les impacts du réchauffement climatique sur l'évolution des paysages en contexte périglaciaire. Les données expérimentales nous montrent (i) l'importance des conditions de saturation de la couche active dans le déclenchement des mécanismes lents et rapides des sols et (ii) l'impact des perturbations des régimes thermiques et hydriques du sol qui modifient à la fois les taux d'érosion et la dynamique des versants périglaciaires. - Lors de précipitations modérées, cryoexpulsion, cryoreptation/gélifluxion et glissements gravitaires sont autant de processus intervenant dans la modification de la morphologie du versant (érosion régressive). - Lors de précipitations intenses, les processus d'érosion rapide type coulées de débris deviennent prédominants, accélérant la dégradation du versant. Ils s'initient systématiquement (i) au niveau des pentes les plus fortes et (ii) en présence d'un pergélisol qui limite l'infiltration de l'eau en profondeur et joue le rôle de plan de glissement. Les taux d'érosion les plus forts sont enregistrés au cours des précipitations les plus intenses. Ces résultats devraient (i) constituer une aide précieuse pour établir une méthodologie de mesure in situ des systèmes périglaciaires et (ii) améliorer la connaissance sur l'évolution morphologique des versants, lorsque le réchauffement climatique augmente à la fois la profondeur du toit du pergélisol et la quantité d'eau apportée aux versants lors des dégels de printemps. Le travail doit désormais se focaliser sur le contrôle exercé par la dynamique de saturation du sol sur les processus d'érosion de versant.

As research continues for the habitation of the Lunar and Martian surfaces, the need for materials for construction of structural parts, mechanical components, and tools remains as a major milestone. The use of in-situ resource utilization (ISRU) techniques is critical due to the financial, physical, and logistical burdens of sending supplies beyond low-Earth orbit. The Bosch process is currently in development as a life support system at the National Aeronautics and Space Administration’s (NASA) Marshall Space Flight Center (MSFC) to regenerate oxygen (O2) from metabolic carbon dioxide (CO2) with the byproduct of elemental carbon (C). The Bosch process presents a possible way of regenerating O2 without the disposal of hydrogen (H2) like the Sabatier. Ionic liquids (ILs) are also studied at MSFC as a means to harvest metallic elements from regolith oxides and meteorites. IL technology provides an energy efficient method of extracting critical manufacturing materials, such as iron (Fe) that could be used for ferrous alloy production. This dissertation seeks to explore the use of Bosch C and IL-Fe for ferrous alloy production through a series of studies. These studies included individually using Bosch C with commercial elements to cast low carbon steel and gray cast iron, investigating as-produced IL-Fe in a laser-based powder bed fusion (PBF-LB) printer to determine IL-Fe metallurgical characteristics, using the IL-Fe composition to design a ductile iron (DI) alloy of similar performance to a commercially available DI alloy, and lastly, refining this DI alloy to produce a DI alloy more representative of an alloy producible from IL-Fe and Bosch byproduct C in a Martian environment. The results presented here suggest that with advances in production rate and control of IL-Fe oxidation, and by providing a sufficient energy grid to operate equipment, a range of high quality DI materials could be manufactured with IL and Bosch process ISRU feedstocks.