In this thesis, the possibility of enabling space-mining for the upcoming decade is explored. Making use of recently-proven reusable rockets, we envision a fleet of spacecraft capable of reaching Near-Earth asteroids. To analyze this idea, the goal of this problem is to maximize the asteroid mass retrieved within a spacecraft max life span. Explicitly, the maximum lifetime of the spacecraft fleet is set at 30 years. A fuel supply-chain is proposed and designed so that each spacecraft is refueled before departing for each asteroid. To maximize access to the number of asteroids and retrievable mass for each mission, we propose launching each mission from an orbit with low escape velocity. The L2-Halo orbit at the libration point in the Earth-Moon system was selected due to its easy access from Low-Earth Orbit and for a cislunar synergy with NASA Gateway. Using data from NASA SmallBody and CNEOS databases, we investigated NEAs in the period between 2030 and 2060 could be captured in the ecliptic plane and returned to L2-Halo with two approaches, MARM-1 and MARM-2. Together, these databases provide all information for every asteroid's close approach known today. Returning the asteroid as a whole is explored in the MARM-1 method, while MARM-2 evaluates the possibility of reaching larger asteroids and returning a fragment of their masses, such that it optimizes the available cargo weight per time of flight of each mission. The following results are compared with previous work from the community. The results show a 96% reduction in the cost per kg, with an enormous increase in retrieved mass. With these results, this thesis shows that not solely energy or dynamic optimization will be responsible for proving space mining feasibility, but rather a combination of those and business best practices. Proving feasibility for space mining is a complex and immense problem. Although this thesis opens new possibilities for future work on the field and sparkes the interest of private endeavors, the final solution for this problem still requires additional exploration. / M.S. / In this thesis, the possibility of enabling space-mining for the upcoming decade is explored. Making use of recently-proven reusable rockets, we envision a fleet of spacecraft capable of reaching Near-Earth asteroids, NEAs. To analyze this idea, the goal of this problem is to maximize the asteroid mass retrieved within a spacecraft max life span. Explicitly, the maximum lifetime of the spacecraft fleet is set at 30 years. A fuel supply-chain is proposed and designed so that each spacecraft is refueled before departing for each asteroid. To maximize access to the number of asteroids and retrievable mass for each mission, we propose launching each mission from an orbit with low escape velocity. A location after the Moon, at the L2-Halo orbit, was selected due to its easy access from Low-Earth Orbit and for a synergy with the proposed new space station at the Moon orbit. Using data from NASA databases, we investigated the asteroids in the period between 2030 and 2060 that could be captured and returned with two approaches, MARM-1 and MARM-2. Together, these databases provide all information for every asteroid's close approach known today. Returning the asteroid as a whole is explored in the MARM-1 method, while MARM-2 evaluates the possibility of reaching larger asteroids and returning a fragment of their masses, such that it optimizes the available cargo weight per time of flight of each mission. The following results are compared with previous work from the community. The results show a 96% reduction in the cost per kg, with an enormous increase in retrieved mass. With these results, this thesis shows that not solely energy or dynamic optimization will be responsible for proving space mining feasibility, but rather a combination of those and business best practices. Proving feasibility for space mining is a complex and immense problem. Although this thesis opens new possibilities for future work on the field and sparkes the interest of private endeavors, the final solution for this problem still requires additional exploration.

The Howardite-Eucrite-Diogenite (HED) meteorites are a suite of basalts, cumulates and breccias which originate from one differentiated parent body, and are linked to the asteroid Vesta. The HEDs are petrologically diverse with a range of major, minor and trace element compositions. Early crystallisation ages are recorded and so the HEDs provide us with a unique snapshot into the early solar system. The aim of this thesis is to investigate the petrogenesis of the eucrites and diogenites by addressing two questions. What is the Bulk Silicate Vesta (BSV) composition? What differentiation and magmatic processes have occurred? Putative BSV compositions were derived from the geochemistry of the meteorites and geophysical observations of Vesta. Series of one-atmosphere experiments and thermodynamic models investigated the BSV phase relations. Olivine crystallised at ~1625 °C, followed by orthopyroxene at ~1350 °C and feldspar at ~1125 °C. Low-Ca pyroxene-melt partition coefficients for the minor and trace elements were measured. The compatibility of the REEs and HFSEs in low- Ca pyroxene increased by a factor of three, as temperature decreased from 1300-1125 °C and calcium content increased from Wo_0.5-Wo₈. These partition coefficients were combined with the observed phase relations to perform geochemical trace element calculations of differentiation and magmatic processes. My results suggest that BSV had an Mg#(100*(Mg/(Mg+Fe²⁺)) between 75-80, > 43 wt. % SiO₂, 2.5 x CI refractory lithophile elements, 0.5 wt. % MnO and 0.75 wt. % Cr₂O₃. A three stage model for Vesta's evolution is suggested. Firstly, extensive if not global partial melting of BSV. Then, equilibrium crystallisation of the mantle and fractional crystallisation of mantle-derived melts produced diogenitic cumulates and eucrite liquids, accounting for the range in major and trace element abundances. The re-equilibration of trapped melt in cumulates is also thought to have occurred. Finally, crustal anatexis produced the range in trace element fractionations seen.

Orbit determination has long relied on the use of the Kalman filter, or specifically the extended Kalman filter, as a means of accurately navigating spacecraft. With the advent of cheaper, more powerful computers more accurate techniques such as the particle filter have been utilized. These Bayesian types of filters have in more recent years found their way to other applications. Dr. Furfaro and B. Gaudet have demonstrated the ability of the particle filter to accurately estimate the angular velocity, homogenous density, and rotation angle of a non-uniformly rotating ellipsoid shaped asteroid. This paper extends that work by utilizing a particle filter to accurately estimate the angular velocity and homogenous density of an ellipsoidal asteroid while simultaneously determining the location and mass of a mass concentration modeled as a point mass embedded within the asteroid. This work shows that by taking measurements in several locations around the asteroid, the asteroid's rotation state and mass distribution can be discerned.

Grains on the surfaces of airless bodies are continually being modified due to their exposure to interplanetary space, a phenomenon known as space weathering. This dissertation uses a multi-faceted approach to understanding space weathering of the lunar and asteroidal surfaces. Chapters 1 and 2 provide an introduction to space weathering and a discussion of the methods employed in this work, respectively. Chapter 3 focuses on the analysis of returned samples from near-Earth asteroid Itokawa using the transmission electron microscope (TEM) and contributes to the first-ever comparison of microstructural and chemical features of space weathering in returned samples from two different airless bodies. This research uses high-resolution imaging and quantitative energy-dispersive x-ray spectroscopy (EDS) measurements to analyze space weathering characteristics in an Itokawa soil grain. These analyses confirm that space weathering is operating on the surface of Itokawa, and that many of the resulting features have similarities to those observed in lunar soils. Results show that while there is evidence that both major constituent space weathering processes are operating on the surface of Itokawa, solar wind irradiation, not micrometeorite impacts, appears to be the dominant contributor to changes in the microstructure and chemistry of surface material. Chapter 4 presents a detailed study of nanophase Fe (npFe) particles in lunar soil samples. For the first-time, the oxidation state of individual npFe particles was directly measured using electron energy-loss spectroscopy (EELS) in the TEM. The results show that npFe particles are oxidizing over their time on the lunar surface, and that the amount of oxidized Fe in the nanoparticles is correlated with soil maturity. The EELS data are also coupled to atomic-resolution imaging, which is used to determine the structure of the nanoparticles, confirming their mineral phase. This work challenges the long-standing paradigm that all npFe particles are composed of metallic Fe and that the chemical composition of these features remains static after their formation. A theoretical modeling investigation of the influence that npFe particles of different oxidation states have on the spectral properties of the material is also presented. The model results show that varied Fe-oxidation states of the nanoparticles can produce subtle changes in the optical properties of the soils, including the degree of reddening and the attenuation of characteristic absorption bands. These findings should be accounted for in future modeling of reflectance spectra. Chapter 5 presents a novel technique for simulating space weathering processes inside the TEM. Using an in situ heating holder, lunar soils were subjected to both slow- (~minutes) and rapid-heating (<seconds) events to simulate micrometeorite impacts. The slow-heating experiments show that npFe forms at ~575 ºC, providing a temperature constraint on initial npFe formation. Lunar soil grains that were subjected to a single, rapid, thermal pulse show the development of npFe particles and vesiculated textures near the grain rim. The vesicles were imaged and the npFe particles were imaged and then mapped with EDS. The oxidation state of the npFe particles was confirmed to be Fe^0 using EELS. Several lunar soil grains were subjected to multiple thermal shocks to simulate longer exposure times on the lunar surface. With each heating cycle, the number and size distribution of the npFe particles changed. The average size of npFe particles increased, and the size distribution became more gaussian after multiple heating events, versus the asymmetric distribution present after only one heating event. These results provide insight into the particle growth dynamics for space weathered soils and could offer a new way to place relative age constraints on grains in lunar soil.Chapter 6 provides a summary of the work presented here, discusses its implications for understanding space weathering processes across the solar system, and presents a perspective on the future of space weathering studies.

The use of origami-based bellows is of interest in fields where traditional metal bellows are incapable of meeting compression, mass, or flexibility constraints. Metal bellows are often used in space applications but frequently complicate spacecraft design. Origami-based bellows capable of meeting design constraints while adequately shielding sensitive spacecraft parts may be advantageous to space mechanism design. The design and testing of a highly compressible origami bellows for harsh environments is described. Several origami patterns were evaluated and the Kresling fold pattern was designed to meet constraints and selected for use in the bellows design. Origami bellows were prototyped in five different materials and tested in fatigue, thermal cycling, ablation, and radiation. Tested bellows show good fatigue life exceeding 100,000 cycles for some materials and resilience to potential harsh environmental conditions such as thermal cycling, abrasion, and high radiation. The bellows can be designed to fit within a given inner and outer diameter and stroke length depending on the design requirements. The origami bellows shows promise for space application and as an adequate replacement for current metal bellows due to its high compressibility and low mass. The design, testing, and fabrication of an origami-based bellows for microgravity drilling is presented. The benefits of origami created an opportunity for application on NASA's Asteroid Redirect Mission (ARM) to protect sensitive parts from debris. Origami-based bellows were designed to fit spacial limitations and meet needed compression ratios. Designs have demonstrated high mass reductions, improved stroke length, greatly decreased stowed volume, improved flexibility, and reduced reaction forces in comparison with traditional metal bellows. Material and design testing demonstrated that a nylon-reinforced polyvinyl fluoride based bellows with an aramid fiber stitched seam is well suited for debris containment in space conditions. Various epoxies were able to maintain an adequate bond with polyvinyl fluoride below expected environmental temperature for bellows mounting to the ARM drill. Asymmetric compression of the bellows can occur at extreme low temperatures and is preventable by balancing stiffness within the structure.

En 2006, Il a été observé que l'astéroïde (234)~Barbara possède une valeur anormalement élevée d’angle d’inversion polarimétrie. Par la suite, d'autres astéroïdes possédant la même caractéristique que Barbara ont été découverts et nommés ``Barbarians'' en référence à (234) Barbara. L'étude de ces astéroïdes constitue le sujet principal de cette thèse ayant pour but de mieux comprendre la raison de cet angle d'inversion plus élevé que la normale. La première hypothèse formulée afin d’expliquer cette anomalie polarimétrique suppose que les astéroïdes Barbarians possèdent une forme fortement irrégulière induisant une réponse polarimétrique particulière. La deuxième hypothèse stipule que les astéroïdes Barbarians possèdent une abondance anormalement élevée d'inclusions riches en aluminium et en calcium. Au cours de cette thèse, nous avons obtenu de nombreuses nouvelles données aussi bien en photométrie, spectroscopie que polarimétrie. Ces nouvelles observations d’astéroïdes ont permis de tester différentes hypothèses formulées précédemment afin d'expliquer l'anomalie polarimétrique observée. Nos observations ont permis d'éliminer une hypothèse faisant appel à une topologie particulière des astéroïdes Barbarians, mais nous avons confirmé et renforcé une autre hypothèse faisant intervenir une composition particulière de ces astéroïdes. Si cette dernière hypothèse était confirmée, cela en ferait des astéroïdes primitifs s'étant formés lors des premières étapes du Système Solaire. Leur étude permettrait donc d'en apprendre plus sur les mécanismes de formation des astéroïdes et la composition de la nébuleuse ayant donné naissance au Système Solaire. Comprendre les astéroïdes Barbarians sert à mieux comprendre les premières étapes de formation du Système Solaire et aussi celles des planètes. / A few years ago, asteroid polarimetry allowed to discover a class of asteroids exhibiting peculiar phase polarization curves, collectively called "Barbarians" from the prototype of this class, the asteroid (234) Barbara. All such objects belong to the L visible plus near infrared based taxonomic class. The anomalous polarization has been tentatively interpreted in terms of high-albedo, spinel-rich Calcium-Aluminum inclusions (CAI) that could be abundant on the surfaces of some of these asteroids, according to their spectral reflectance properties and to analogies with CO3/CV3 meteorites. Such CAIs are among the oldest mineral assemblages ever found in the Solar System. Barbarians' surfaces could therefore be rich in this very ancient material and bring information on the early phases of planetary formation. During this thesis, a systematic campaign for photometric, polarimetric and spectroscopic characterization has been conducted. These observation campaigns allowed improving our general knowledge about these peculiar asteroids and highlighting the link between polarization and polarimetric properties. Our observation also allowed discarding the hypotheses involving peculiar shape for these asteroids. However, as it was suggested, a link between the presence of CAI and the polarimetric response was found. Our observations show that the relative abundance of CAI is correlated with the polarimetric inversion angle. This is the first time that a direct link between polarimetric and spectroscopic properties is found.

Astronomy is a data heavy field driven by observations of remote sources reflecting or emitting light. These signals are transient in nature, which makes it very important to fully utilize every observation. This however is often difficult due to the faintness of these observations, often are only slightly above the level of observational noise. We present new or adapted methodologies for dealing with these low signal-to-noise scenarios, along with practical examples including determining exoplanet physical properties, periodicities in asteroids, and the rotational and orbital properties of the multiple asteroid system 2577 Litva.

Micrometeoroids and orbital debris (MMOD) is a growing issue with international importance. Micrometeoroids are naturally occurring fragments of rock and dusk that exist throughout the solar system. Orbital debris is human made material like rocket bodies, paint flakes, and the effluent of spacecraft collisions. Even small MMOD particles on the order of 1 cm in diameter have the potential to destroy critical spacecraft systems. Because of this, MMOD is a threat to all spacecraft in orbit. Even governments that most sternly oppose US international policy have a stake when it comes to minimizing MMOD flux. Space-based assets are essential to support the growing demand for high-capacity communications networks around the world. These networks support services that civilian and military users have grown accustomed to using on a daily basis: Global Positioning System (GPS), Satellite Radio, Internet Backhaul, Unmanned Areal Vehicles (UAVs), and Reconnaissance Satellites [Figure \ref{figure:skynet}]. A sudden loss of these services could degrade the warfighter's capabilities and cripple commercial enterprises that rely on these technologies. Manned space efforts like the International Space Station (ISS) could also suffer as a result of increased MMOD flux.

Autonomous proximity operations are the future of Deep space robotic exploration for searchof life, mining for resources and to establish outposts. Part of that future depends on howwell the spacecraft is capable to navigate around the complex environment of the smallcelestial body. The shift from huge monolithic spacecraft to a lightweight distributed Spacesystems has opened up a new opportunity for early characterization and global mappingmissions around these bodies. This project aims to contribute to help solve a part of thedream, wherein multiple spacecrafts operate cooperatively in proximity of small celestialbodies. To that extent, a 6 DoF controlled software-in-loop simulation is performed withsimulated optical sensors and IMU on board the spacecraft for verification of the controlledcooperative operation of two spacecrafts in a Leader-Follower configuration.

No description available.