Theses and Dissertations from UMD
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New submissions to the thesis/dissertation collections are added automatically as they are received from the Graduate School. Currently, the Graduate School deposits all theses and dissertations from a given semester after the official graduation date. This means that there may be up to a 4 month delay in the appearance of a give thesis/dissertation in DRUM
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Item On the Dynamics of Binary Asteroids Applied to DART Mission Target (65803) Didymos(2022) Agrusa, Harrison Fitzgerald; Richardson, Derek C; Astronomy; Digital Repository at the University of Maryland; University of Maryland (College Park, Md.)NASA’s Double Asteroid Redirection Test (DART) mission will be the first full-scale demonstration of a kinetic impactor for planetary defense. On September 26, 2022, the DART spacecraft is expected to impact Dimorphos, the secondary component of the Didymos binary asteroid system. The DART impact will reduce Dimorphos’s relative orbital velocity, shrinking both its semimajor axis and orbit period. The mutual orbit period will then be measured us- ing ground- and space-based observations in order to deduce the momentum transfer efficiency, which is an important parameter in planetary defense that has never been measured experimentally at a realistic scale. This thesis comprises a set of studies on the spin and orbital dynamics of the Didymos system conducted in support of the DART mission. Owing to the close proximity of Didymos and Dimorphos and their irregular shapes, the mutual dynamics are non-Keplerian and exhibit a high degree of spin-orbit coupling, which often requires the use of specialized numerical methods to model the system. First, we conducted a benchmarking and sensitivity study to identify the best simulation codes for future DART-supported studies and to understand how small perturbations in the initial conditions can affect the resulting dynamical evolution of the system. Then, we demonstrated that Dimorphos can enter a wide range of post-impact spin states, including possible chaotic non-principal axis rotation, depending on its shape and the amount of momentum transferred by the DART impact. We then explored the implications of an excited spin state, including the possibility of ongoing granular motion on Dimorphos’s surface resulting from the orbital perturbation induced by the DART impact. This thesis is focused predominantly on the dynamics of the Didymos binary. However, there are many other binary systems among the near-Earth asteroid population with similar physical and dynamical properties, making the results presented here relevant to the NEA binary population in general.Item SIMULATION OF MAGNETIC GRANULAR MEDIA USING OPEN SOURCE SOFT SPHERE DISCRETE ELEMENT METHOD(2021) Leps, Thomas; Christine, Hartzell; Aerospace Engineering; Digital Repository at the University of Maryland; University of Maryland (College Park, Md.)Magnetic granular media were investigated using a mutual dipole magnetic model integrated into the open source Soft Sphere Discrete Element Method (DEM) framework LAMMPS and LIGGGHTS. Using the magnetic model and the contact force models from LIGGGHTS, we simulated shear behavior of MagnetoRheological Fluids (MRF). We found that the size distribution of simulated particles significantly affects the qualitative and quantitative behavior of MRF in a simple shear cell. Additionally, including cohesion, rolling resistance, friction and other contact forces affect the simulated shear behavior. By using a high fidelity contact force model along with an accurate size distribution and the mutual dipole magnetic model we were able to accurately match experimental data for an example MRF.We used the DEM model to aid in the development of a novel MRF valve operating on an alternative MRF behavior. Our jamming, MRF valve holds pres- sure through stable, but reversible jamming in the flow path, and is actuated by electropermanent magnets, which require no quiescent current to maintain their magnetization states. These valves do not require the large power draw of con- ventional MRF valves to maintain their state. We were able to accurately predict the experimental jamming behavior of the MRF valve using Finite Element Analysis and LIGGGHTS with magnetization, further validating the model with a non-linear, non-continuum behavior. Our jamming MRF valve was demonstrated in a multi- segmented, elastomeric robot, actuated using MRF. Using the magnetic DEM model coupled with self-gravity, the effects of mag- netism on rubble pile magnetic asteroids were examined. We simulated formation, and disruption of metallic asteroids with remnant magnetizations using LAMMPS with permanent dipoles. We found that rubble pile asteroids, formed from clouds of magnetized grains, coalesce more quickly, and have higher porosities than aster- oids coalesced from unmagnetized grains. Distortion and disruption was affected by magnetization during simulated YORP spin-up. Large fragments with high aspect ratios and low densities were formed from highly magnetized asteroids after disrup- tion, matching the shapes of suspected metallic small bodies. Simulations of grain avalanching on the surface of magnetized asteroids found additional morphological differences from their unmagnetized counterparts, with reduced densities, increased angles of repose, and cornicing.Item Petrologic, Geochemical, and Spectral Characteristics of Oxidized Planetary Differentiation(2021) Crossley, Samuel Dean; Sunshine, Jessica M; Ash, Richard D; Geology; Digital Repository at the University of Maryland; University of Maryland (College Park, Md.)Meteorites provide evidence that planetary formation occurred across a wide range of oxidation environments in the early Solar System. While the process of differentiation for many reduced, oxygen-poor assemblages has been thoroughly explored, significantly less is known about how differentiation occurred in more oxidized regions of the Solar System. Results from petrologic and geochemical investigations of oxidized chondrites (Rumurutiites) and primitive achondrites (brachinites) reveal that significant mineralogic differences occur with increasing degrees of oxidation. As a consequence, the differentiation pathways of oxidized and reduced assemblages diverge during the earliest stages of partial melting. While reduced materials differentiate to form a basaltic crust, magnesian peridotite mantle, and metallic core, oxidized materials may instead form felsic crusts, ferroan peridotite mantles, and sulfide-dominated cores. These pathways are evident in distinct siderophile trace element systematics for oxidized and reduced endmembers of the brachinite meteorite family. The compositions of olivine between oxidation endmembers are resolvable using remote sensing techniques that are applicable to asteroids. Most olivine-dominated asteroids examined in this work are consistent with having formed in oxidized environments, similar to R chondrites and brachinites, or in even more oxidizing environments not recorded among the meteoritic record. This provides strong evidence that environments capable of supporting oxidized, sulfide-dominated core formation are widespread among asteroidal materials. Several of these asteroids are likely mantle restites, based on their olivine composition and the estimated abundances of pyroxene. The predominance of oxidized over reduced environments among olivine-dominated asteroids is likely related to their respective petrogenetic histories: reduced assemblages must reach and sustain much higher temperatures to fully melt and segregate their pyroxene contents from olivine, which requires larger and earlier-accreted parent bodies. Consequently, sampling reduced mantle restites without significant pyroxene contamination would require catastrophic parent body destruction without mixing crustal and mantle materials. Oxidized materials, in contrast, have much higher initial olivine/pyroxene ratios, and thus are much more prone to producing asteroids dominated by olivine.Item A MODEL TO PREDICT THE SIZE OF 3D REGOLITH CLUMPS ON PLANETARY BODIES(2020) Patel, Anand Vijaykumar; Hartzell, Christine M; Aerospace Engineering; Digital Repository at the University of Maryland; University of Maryland (College Park, Md.)Prior investigations of the behavior of regolith on the surface of planetary bodies has considered the motion and interactions of individual grains. Recent work has shown the significance of cohesion in understanding the behavior of planetary regolith, especially on small, airless bodies. Surficial regolith grains may detach from a planetary body due to a variety of phenomena, including aeolian effects, spacecraft operations, micrometeoroid bombardment and electrostatic lofting. It is well known in terrestrial powder handling that cohesive powders tend to form clumps. We present an analytical theory for the size of regolith clumps that are likely to form and be easier to detach from a surface than their constituent grains, assuming monodisperse, spherical grains. The model predictions are significant for our interpretation of the surface of asteroids, as well as understanding a variety of phenomena on planetary bodies and designing of sampling spacecraft.