Thesis (Ph. D.)--University of Missouri-Columbia, 1996. / Typescript. Vita. Includes bibliographical references. Also available on the Internet.

Thesis (M.E.)--University of Canterbury, 2008. / Typescript (photocopy). Includes bibliographical references (leaves 102-104). Also available via the World Wide Web.

Mémoire (M.Eng.)--Université du Québec à Chicoutimi, 1996. / Document électronique également accessible en format PDF. CaQCU

Thesis (M.S.)--University of Wisconsin--Madison, 1966. / eContent provider-neutral record in process. Description based on print version record. Includes bibliographical references.

Thesis (M.S.)--University of Wisconsin--Madison, 1970. / eContent provider-neutral record in process. Description based on print version record. Includes bibliographical references.

Thesis (M. Eng.)(Mechanical)--University of Pretoria, 2005. / Title from opening screen (viewed Mar. 20, 2006). Includes summary. Mode of access: World Wide Web.

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In laboratory experiments, I study strongly-coupled dusty plasma levitated in a glow-discharge plasma. Dusty plasma is an arrangement of small dust particles in a plasma background of electrons, ions, and neutral gas. The dust particles are negatively charged because they collect electrons and ions from the background plasma. Depending on the experimental setup, the plasma's electric field can help to balance the dust particles against gravity. The high dust charge causes dust particles to repel each other, while confinement forces prevent their escape. The dust particles cannot easily move past one another, and instead organize themselves into highly-ordered structures. The neutral gas also plays a key role in these experiments. Depending on the relative motion between gas and dust particles, the neutral gas can either impede dust motion or it can drive the dust into motion. In this thesis, I report the findings of three separate experiments. In the first experiment, I use a spherically-shaped dusty plasma (Yukawa ball) as an indicator of a flow of neutral gas, called thermal creep flow. In the second and third experiments, I study naturally occurring dust-density waves, which propagate within the volume of a dusty plasma that has many horizontal layers. In Ch.2 of this thesis, I study thermal creep flow (TCF), which is a flow of gas driven by a temperature gradient along a solid boundary. Stripes on a glass box are heated by laser beam absorption, leading to both TCF and a thermophoretic force. A stirring motion of the dust particle suspension is observed. By eliminating all other explanations for this motion, I conclude that TCF at the boundary couples by drag to the bulk gas, causing the bulk gas to flow, thereby stirring the suspension of dust particles. This result provides an experimental verification that TCF in the slip-flow regime causes steady-state gas flow in a confined volume. In Ch.3, I observe the growth of a naturally occurring dust-density wave (DDW) using high-speed imaging. This low-frequency wave (∼ 25 Hz) grows in amplitude as it propagates downward through a dusty plasma. I measure the wave's linear growth rate using a phase-sensitive analysis method. For the conditions studied here, the growth rate increases as gas pressure decreases. At a critical gas pressure that I observe, a balance between an ion-flow instability and dissipation by neutral gas drag determines a threshold for wave propagation. A linear dispersion relation is derived, taking into account effects of strong coupling, to compare to the experiment. In Ch.4, I observe the development of nonlinearity in the naturally occurring dust-density wave by measuring harmonics of the fundamental. Using high-speed imaging, I measure amplitudes, wave numbers and growth rates for the fundamental and its harmonics. The amplitudes of the harmonics exhibit a strong exponential increase with diminishing gas pressure, and they saturate at lower gas pressures. My measurements show that the wave numbers and growth rates of harmonics are near integer multiples of the fundamental.

The circumgalactic medium (CGM), loosely defined as the region between a galaxy disk and its virial radius, has long been of interest to astronomers and astrophysicists because it acts as an interface between galaxies and their surroundings. Studying it, therefore, gives us hints of how gas flows between galaxies and the intergalactic medium (IGM), fueling star formation for instance. This thesis addresses some of the current and future observation, analysis and instrumentation challenges that should be tackled for a better understanding of the CGM. Chapter 1 is an overview of science related to the CGM and of instruments that our lab works on: the Circumgalactic Hydrogen-Alpha Spectrograph (CHaS) and the Faint Intergalactic-medium Redshifted Emission Balloon (FIREBall). It sets the ground for a better understanding of the science discussed in subsequent chapters. CHaS is an IFU spectrograph installed on a 2.4 m telescope at the MDM Observatory in Arizona (Melso et al. 2022). It has high sensitivity and high spectral resolution, and it collects individual spectra from points across our targets using a microlens array, allowing us to make detailed spectral maps of observed astronomical objects. FIREBall is a balloon-born UV multi-object spectrograph, allowing us to look at yet another emission line prominent in the CGM. In this thesis, we will focus on what a future FIREBall detector might look like. Chapters 2 and 3 present data collected with CHaS in November 2021 from two very distinct objects: NGC 6946 (the Fireworks galaxy) and M76 (the Little Dumbbell nebula). Both chapters address how we process spectral data from CHaS images and the subsequent making of velocity maps. Using CHaS images, we tackle anomalous gas motion and formations in both targets. We compared the data presented in both chapters to previous literature, showing that CHaS velocity maps were more detailed and complimented previous findings. NGC 6946 is known for being a prolific star forming galaxy and also for having holes in its HI distribution, which have historically been attributed to the expansion and bursting of gas bubbles. In Chapter 2, we find that the motion around these holes is indeed consistent with expanding bubbles and galactic fountains on their edges, with velocities in the -20 km/s to 20 km/s range, consistent with what Boomsma et al. (2008) found, going up to +/-60 km/s, similar to the velocities found by Efremov et al. (2002). We also found that Long et al. (2019)'s supernova remnants candidates catalog had a clear position correlation with the boundaries of different holes in the Boomsma et al. (2008) HI hole catalog, suggesting that these holes might indeed be related to gas bubbles resulting from supernova explosions. The Little Dumbbell nebula, on the other hand, show its own set of anomalies. M76 is a butterfly planetary nebula with a central torus and two polar lobes. We find that these lobes are not completely symmetric. In fact, the wester lobe is more rounded and the eastern one is more stretched and fragmented. From our velocity maps, we propose a couple of explanations for how the ISM might interact with the nebula both in the core star's AGB phase and after the nebula is formed to give M76 its shape. Both explanations vary depending on the assumed direction of motion of the star in it its AGB phase, but both are consistent with models by Villaver, Manchado and García-Segura (2012) and Wareing et al. (2007). Moreover, we compare our data to those of other authors and find similar velocity ranges around an axis going from one lobe to another as spectral maps made by Ramos-Larios et al. (2017) and Bryce et al. (1996). Departing from observational data analysis, Chapter 4 focuses on how we can probe further into the CGM by upgrading existing instruments, turning commonplace condensed matter methods into tools for astrophysics. More specifically, Chapter 4 discusses the possibility of switching FIREBall's current UV sensitive emCCD detectors, which rely on coating to be visible-blind and on cryogenic equipment that is heavy for a balloon flight, for devices made out of hexagonal boron nitride (hBN). hBN's main energy bandgap overlaps with the emission lines that FIREBall is interested in capturing, and it can be combined with graphene (which is isomorphic to hBN) to make high quality, quantum efficient devices. While we weren't able to finish full devices, Chapter 4 discusses their fabrication in detail as well as how our Siesta SISL simulations show that even small device defects might be acceptable for a detector. The chapter ends with considerations about how one might fit individual devices as multi-pixel detectors.