The number of objects occupying orbital regimes beyond Geosynchronous Earth Orbit and cislunar space are expected to grow in the coming years; Especially with the Moon reemerging as latest frontier in the race for space exploration and technological superiority. In order to support this growth, new methods of autonomously navigating in cislunar space are necessary to reduce demand and reliance on ground based tracking infrastructure. Periodic orbits about the first libration point offer favorable vantage points for scientific or military spacecraft missions involving the Earth or Moon. This thesis develops a new autonomous spacecraft navigation method for cislunar space and analyzes its performance applied to Lyapunov and halo orbits around $L_1$. This method uses existing lunar ranging retroreflectors (LRRR) installed on the Moon's surface in the 1960s and 1970s. A spacecraft can make laser ranging measurements to the LRRR to estimate its orbit states. A simulation platform was created to test this concept in the circular restricted three body problem and evaluate its performance. This navigation method was found to be successful for a subset of Lyapunov and halo orbits when cycling the five measurement targets. Simulation data showed that sub-kilometer position estimation and sub 2 centimeter per second velocity accuracies are achievable without receiving any state updates from external sources. / Master of Science / The number of objects occupying the space between the Earth and Moon (cislunar space) is expected to grow in the coming years as the Moon regains popularity in the latest race for space exploration and technological superiority. In order to support this growth, new methods of determining a spacecraft's position and velocity while in this region of space are necessary to reduce demand and dependence on Earth based methods, which have historically relied upon. Repeating orbits around the equilibrium point between the Earth and Moon provide valuable observation points for scientific and military spacecraft missions. This thesis develops a new spacecraft navigation method for cislunar space and analyzes how well it performs in two different types of orbits, Lyapunov and halo orbits. This method uses existing laser reflector panels that were installed on the Moon's surface in the 1960s and 70s. A spacecraft can use these panels to make range or distance measurements in order to estimate its position and velocity. Software was written to simulate the motion of a spacecraft as it is acted on by gravity from the Earth and Moon. Different scenarios were then simulated and used to test this concept and evaluate its performance. Lunar laser ranging was found to be successful for a some Lyapunov and halo orbits when switching between the five different reflector panels on the Moon. Data generated from the simulations show that position can be estimated with errors less than SI{1}{kilo meter}, and velocity error on the order of a few centimeters per second, all without receiving any additional information from Earth based systems.

No description available.

Being able to identify fuel efficient transfers between orbits is critical to planning and executing missions involving spacecraft. With a renewed focus on missions in cislunar space, identifying efficient transfers in the dynamical environment characterized by the Circular Restricted Three-Body Problem (CR3BP) will be especially important, both now and in the immediate future. The focus of this thesis is to develop a methodology that can be used to identify a valid low-cost transfer between a variety of orbits in the CR3BP. The approach consists of two distinct parts. First, tools related to dynamical systems theory and manifolds are used to create an initial set of possible transfers. An optimization scheme is then applied to the initial transfers to obtain an optimized set of transfers. Code was developed in MATLAB to implement and test this approach. The methodology and its implementation were evaluated by using the code to identify a low-cost transfer in three different transfer cases. For each transfer case, the best transfers from each set were compared, and important characteristics of the transfers in the first and final sets were examined. The results from those transfer cases were analyzed to determine the overall efficacy of the approach and effectiveness of the implementation code. In all three cases, in terms of cost and continuity characteristics, the best optimized transfers were noticeably different compared to the best manifold transfers. In terms of the transfer path identified, the best optimized and best manifold transfers were noticeably different for two of the three cases. Suggestions for improvements and other possible applications for the developed methodology were then identified and presented. / Master of Science / Being able to identify fuel efficient transfers between orbits is critical to planning and executing missions involving spacecraft. With a renewed focus on lunar missions, identifying efficient transfers between orbits in the space around the Moon will be especially important, both now and in the immediate future. The focus of this thesis is to develop a methodology that can be used to identify a valid low-cost transfer between a variety of orbits in the space around the Moon. The approach was evaluated by using the code to identify a low-cost transfer in three different transfer cases. The results from those transfer cases were analyzed to determine the overall efficacy of the approach and effectiveness of the implementation code. Suggestions for improvements and other possible applications for the developed methodology were then identified and presented.

Radioactive beams of 8Li and 6He were produced using the double superconducting solenoid system of RIBRAS (Radioactive Ion Beams in Brasil) with a primary beam of 7Li of Elab = 30 MeV, at the São Paulo Pelletron Accelerator. The production reactions were 9Be(7Li, 8Li)8Be and 9Be(7Li, 6He)10B. The angular distributions of the elastic scattering of the 8Li radioactive beam of 26.0 MeV and 6He radioactive beam of 23.0 MeV were measured on 51V target of 1.9 mg/cm2.The elastic scattering angular distributions were analyzed using Optical Model, where the real and imaginary parts are described through a Non-Local Interaction Model called São Paulo Potential . The results were compared with the data present in the literature. The largest cross section, particularly for the halo 6He, shows evidence of the importance of the break up for these medium mass systems. [1]R. Lichtenthaler et al, Eur. Phys. J. A 25,s01,733 (2005); [2]L.C. Chamon et al, Phys. Rev. C66 (2002) 014610. / Radioactive beams of 8Li and 6He were produced using the double superconducting solenoid system of RIBRAS (Radioactive Ion Beams in Brasil) with a primary beam of 7Li of Elab = 30 MeV, at the São Paulo Pelletron Accelerator. The production reactions were 9Be(7Li, 8Li)8Be and 9Be(7Li, 6He)10B. The angular distributions of the elastic scattering of the 8Li radioactive beam of 26.0 MeV and 6He radioactive beam of 23.0 MeV were measured on 51V target of 1.9 mg/cm2.The elastic scattering angular distributions were analyzed using Optical Model, where the real and imaginary parts are described through a Non-Local Interaction Model called São Paulo Potential . The results were compared with the data present in the literature. The largest cross section, particularly for the halo 6He, shows evidence of the importance of the break up for these medium mass systems. [1]R. Lichtenthaler et al, Eur. Phys. J. A 25,s01,733 (2005); [2]L.C. Chamon et al, Phys. Rev. C66 (2002) 014610.

Three scenarios regarding a target man's moral behavior were used to examine 'religious halo' 'religious boomerang', and a 'halo recovery' effect. Initially, participants rated a male target in response to his religious affiliation. Secondly, participants rated the male target following an act of infidelity. Finally, participants provided ratings of the male target with the knowledge that the target received forgiveness from significant others. Results indicated that participants did not discriminate based on knowledge of the target's religious affiliation but did reject the target following an act of infidelity. New to this research, however, was discovery of a 'halo recovery' where participants were again accepting of a target following forgiveness from his wife and church leaders. These results varied from previous findings that suggested that participants' religious affiliation primarily influenced judgments of moral behavior.

We present the results of a new and high sensitivity study of the neutral hydrogen (HI) gas in three early type edge-on spiral galaxies, NGC 4157, NGC 3600 and NGC 2683. All three galaxies reveal HI disks that extend nearly or more than twice the length of the optical disk, which ubiquitously reveal asymmetries and warps. We model each galaxy using a three-dimensional kinematic model to derive the empirical parameters of the density distribution functions and rotation curves. A Gaussian function is unanimously found to best represent the density distribution in the plane of the galaxies. We also find that there is in fact a thick HI disk extending into the halo of two of three of these galaxies with scale heights on kpc. scales. This gas suggests the existence of two separate widespread components: a thin, high intensity disk component, normally rotating, and a vast, low intensity halo component, rotating at slower velocities with respect to the disk. This vertical velocity gradient is perhaps our most significant finding in addition to the discovery of the two new HI halos. We also find an unevenly distributed small-scale component of the gas in the form of shell-like and filamentary structures that extend from the disk into the halo. In all three systems we find unique kinematic and structural peculiarities including an HI disk extending four times the optical disk, a declining rotation curve, a companion, expanding bubbles, disk warps, etc. Several physical parameters are derived such as neutral hydrogen and dynamic masses, systemic velocities, HI radii, HI halo masses, etc. All of our findings are investigated and discussed in depth for each of the three galaxies. / Thesis (Master, Physics, Engineering Physics and Astronomy) -- Queen's University, 2009-09-03 19:47:31.786

Today, it is well known that galaxies like the Milky Way consist not only of stars but also of gas and dust. The galactic halo, a sphere of gas that surrounds the stellar disk of a galaxy, is especially interesting. It provides a wealth of information about in and outflowing gaseous material towards and away from galaxies and their hierarchical evolution. For the Milky Way, the so-called high-velocity clouds (HVCs), fast moving neutral gas complexes in the halo that can be traced by absorption-line measurements, are believed to play a crucial role in the overall matter cycle in our Galaxy. Over the last decades, the properties of these halo structures and their connection to the local circumgalactic and intergalactic medium (CGM and IGM, respectively) have been investigated in great detail by many different groups. So far it remains unclear, however, to what extent the results of these studies can be transferred to other galaxies in the local Universe. In this thesis, we study the absorption properties of Galactic HVCs and compare the HVC absorption characteristics with those of intervening QSO absorption-line systems at low redshift. The goal of this project is to improve our understanding of the spatial extent and physical conditions of gaseous galaxy halos in the local Universe. In the first part of the thesis we use HST /STIS ultraviolet spectra of more than 40 extragalactic background sources to statistically analyze the absorption properties of the HVCs in the Galactic halo. We determine fundamental absorption line parameters including covering fractions of different weakly/intermediately/highly ionized metals with a particular focus on SiII and MgII. Due to the similarity in the ionization properties of SiII and MgII, we are able to estimate the contribution of HVC-like halo structures to the cross section of intervening strong MgII absorbers at z = 0. Our study implies that only the most massive HVCs would be regarded as strong MgII absorbers, if the Milky Way halo would be seen as a QSO absorption line system from an exterior vantage point. Combining the observed absorption-cross section of Galactic HVCs with the well-known number density of intervening strong MgII absorbers at z = 0, we conclude that the contribution of infalling gas clouds (i.e., HVC analogs) in the halos of Milky Way-type galaxies to the cross section of strong MgII absorbers is 34%. This result indicates that only about one third of the strong MgII absorption can be associated with HVC analogs around other galaxies, while the majority of the strong MgII systems possibly is related to galaxy outflows and winds. The second part of this thesis focuses on the properties of intervening metal absorbers at low redshift. The analysis of the frequency and physical conditions of intervening metal systems in QSO spectra and their relation to nearby galaxies offers new insights into the typical conditions of gaseous galaxy halos. One major aspect in our study was to regard intervening metal systems as possible HVC analogs. We perform a detailed analysis of absorption line properties and line statistics for 57 metal absorbers along 78 QSO sightlines using newly-obtained ultraviolet spectra obtained with HST /COS. We find clear evidence for bimodal distribution in the HI column density in the absorbers, a trend that we interpret as sign for two different classes of absorption systems (with HVC analogs at the high-column density end). With the help of the strong transitions of SiII λ1260, SiIII λ1206, and CIII λ977 we have set up Cloudy photoionization models to estimate the local ionization conditions, gas densities, and metallicities. We find that the intervening absorption systems studied by us have, on average, similar physical conditions as Galactic HVC absorbers, providing evidence that many of them represent HVC analogs in the vicinity of other galaxies. We therefore determine typical halo sizes for SiII, SiIII, and CIII for L = 0.01L∗ and L = 0.05L∗ galaxies. Based on the covering fractions of the different ions in the Galactic halo, we find that, for example, the typical halo size for SiIII is ∼ 160 kpc for L = 0.05L∗ galaxies. We test the plausibility of this result by searching for known galaxies close to the QSO sightlines and at similar redshifts as the absorbers. We find that more than 34% of the measured SiIII absorbers have galaxies associated with them, with the majority of the absorbers indeed being at impact parameters ρ ≤160 kpc. / Galaxien bestehen nicht nur aus Planeten und Sternen, sondern sind u.a. auch von einer Hülle aus Gas und Staub, dem Halo, umgeben. Dieser Halo spielt für die Entwicklung der Galaxie eine zentrale Rolle, da er mit der galaktischen Scheibe wechselwirken kann. Für das Verständnis des galaktischen Materiekreislaufs ist es daher entscheidend, die Prozesse und Vorgänge sowie das Zusammenspiel der verschiedenen Gasphasen in diesem Übergangsbereich zum intergalaktischen Medium charakterisieren und verstehen zu können. In der vorliegenden Arbeit werden lokale Phänomene, die sogenannten Hochgeschwindigkeitswolken (HVCs), im Halo der Milchstraße mit Hilfe des Hubble-Weltraumteleskops analysiert und ausgewertet. Im Gegensatz zu dem normalen Halo Gas bewegen sich diese HVCs mit ungewöhnlich hohen Geschwindigkeiten durch die ̈ äußeren Bereiche der Milchstraße. Sie passen daher nicht in das Galaktische Ge- schwindigkeitsmodell und stellen eine eigene, wichtige Klasse von Objekten dar, welche mit der Galaxie wechselwirken und diese beeinflussen. Für die Analyse dieser HVCs werden mehr als 40 Spektren von extragalaktischen Hintergrundquellen statistisch untersucht, um u.a. den Bedeckungsanteil von verschiedenen niedrig-/mittel- und hochionisierten Metallen zu ermitteln. Wegen der Ähnlichkeit der Ionisationsparameter von einfach ionisiertem Silizium, SiII, und einfach ionisiertem Magnesium, MgII, ist es möglich, den Beitrag von HVCs zum Wirkungsquerschnitt von starken MgII Absorbern im lokalen Universum zu bestimmen. Es stellt sich heraus, dass, würde man von außen auf die Milchstraße schauen, Galaktische HVCs etwa 52 % zum totalen Wirkungsquerschnitt von starken MgII Absorptionssystemen in der Milchstraße beitragen. Weiterhin ergibt sich, dass nur etwa ein Drittel der starken MgII Absorptionssysteme in der Umgebung von Milchstraßen-ähnlichen Galaxien als HVC Gegenstücke identifziert werden kann. Betrachtet man die große Anzahl an bekannten MgII Absorptionssystemen folgt daraus, dass das HVC-Phänomen nicht alleine auf unsere Galaxie beschränkt ist, sondern im Gegenteil, weit verbreitet zu sein scheint. Weiterhin werden die Eigenschaften von Metallsystemen bei niedriger Rotverschiebung in Quasarspektren analysiert. Die Suche nach extragalaktischen Metallsystemen in einer Vielzahl von Spektren und deren statistische Auswertung bezogen auf ihre Ursprungsgalaxien ermöglicht es, neue Erkenntnisse über die typische Struktur von Halos Milchstraßen-ähnlicher Galaxien zu erlangen. Eine der Hauptfragestellungen ist die Identifizierung von entfernten Metallsystemen als HVC-Analoga. Dazu wurden weitere Quasarspektren des Hubble-Teleskops ausgewertet und mit den Ergebnissen über Galaktische HVCs verglichen. Es zeigt sich hierbei, dass z.B. in der Säulendichteverteilung von neutralem Wasserstoff eine deutliche zweikomponentige Struktur zu erkennen ist. Diese könnte das Resultat von zwei verschiedenen Absorber Populationen sein, wobei eine HVC-ähnliche Eigenschaften aufweist. Diese Absorptionssysteme besitzen im Mittel sehr ähnliche Eigenschaften wie Galaktische Absorber, z.B. in Bezug auf die Eigenschaften des Gases oder dessen Zusammensetzung. Das impliziert u.a., dass sich auch dazugehörige Galaxien innerhalb eines bestimmten Abstandes um diese Absorber befinden sollten. Diese Vermutung wird anhand der Daten exemplarisch für zweichfach ionisiertes Silizium, SiII, untersucht. Es stellt sich heraus, dass sich in mehr als 34 % der Fälle zugehörige Galaxien bei SiIII Absorbern befinden, wobei die Mehrheit sogar innerhalb des von uns ermittelten mittleren Detektionsradius von 160 kpc zu finden ist. Allgemein können wir viele Hinweise darauf finden, dass das HVC-Phänomen nicht nur auf die Milchstraße beschränkt, sondern weit verbreitet ist. Zusätzlich scheinen Metallsysteme in Quasarspektren gute Indikatoren für HVC-Analoga in der Umgebung von anderen entfernten Galaxien zu sein.

Radioactive beams of 8Li and 6He were produced using the double superconducting solenoid system of RIBRAS (Radioactive Ion Beams in Brasil) with a primary beam of 7Li of Elab = 30 MeV, at the São Paulo Pelletron Accelerator. The production reactions were 9Be(7Li, 8Li)8Be and 9Be(7Li, 6He)10B. The angular distributions of the elastic scattering of the 8Li radioactive beam of 26.0 MeV and 6He radioactive beam of 23.0 MeV were measured on 51V target of 1.9 mg/cm2.The elastic scattering angular distributions were analyzed using Optical Model, where the real and imaginary parts are described through a Non-Local Interaction Model called São Paulo Potential . The results were compared with the data present in the literature. The largest cross section, particularly for the halo 6He, shows evidence of the importance of the break up for these medium mass systems. [1]R. Lichtenthaler et al, Eur. Phys. J. A 25,s01,733 (2005); [2]L.C. Chamon et al, Phys. Rev. C66 (2002) 014610. / Radioactive beams of 8Li and 6He were produced using the double superconducting solenoid system of RIBRAS (Radioactive Ion Beams in Brasil) with a primary beam of 7Li of Elab = 30 MeV, at the São Paulo Pelletron Accelerator. The production reactions were 9Be(7Li, 8Li)8Be and 9Be(7Li, 6He)10B. The angular distributions of the elastic scattering of the 8Li radioactive beam of 26.0 MeV and 6He radioactive beam of 23.0 MeV were measured on 51V target of 1.9 mg/cm2.The elastic scattering angular distributions were analyzed using Optical Model, where the real and imaginary parts are described through a Non-Local Interaction Model called São Paulo Potential . The results were compared with the data present in the literature. The largest cross section, particularly for the halo 6He, shows evidence of the importance of the break up for these medium mass systems. [1]R. Lichtenthaler et al, Eur. Phys. J. A 25,s01,733 (2005); [2]L.C. Chamon et al, Phys. Rev. C66 (2002) 014610.

Depuis leur découverte au milieu des années quatre-vingt, les noyaux à halo n'ont cessé d'intriguer et de fasciner. Cette découverte a été rendue possible par le développement de faisceaux d'ions radioactifs au cours des années septante. Cette performance a ouvert le champ de l'exploration des propriétés des noyaux atomiques aux frontières de la stabilité. Les noyaux à halo présentent une taille beaucoup plus grande que prévue par l'hypothèse communément adoptée du noyau sphérique et seraient constitués d'un coeur, qui a les propriétés d'un noyau normal, auquel un ou deux neutrons qui forment le halo seraient faiblement liés. Cette propriété bouleverse complètement l'image traditionnelle du noyau atomique, celle d'un mélange quasiment homogène de protons et de neutrons. Les noyaux à halo ont tendance à facilement se dissocier lorsqu'ils entrent en collision avec un noyau cible. Leurs réactions de dissociation constituent donc un formidable outil expérimental pour étudier leurs propriétés. Cependant l'analyse de telles réactions nécessite une description précise du processus de collision. A cette fin, nous avons développé un nouveau modèle de réaction: l'approximation eikonale dynamique. Il s'agit d'une méthode purement quantique qui combine les avantages des approximations eikonale traditionnelle et semi-classique. Elle prend en compte aussi bien les effets dynamiques du mouvement interne du projectile que les interférences quantiques entre les trajectoires. Elle conduit à la résolution d'une équation de Schrödinger approchée similaire à celle de l'approximation semi-classique avec trajectoires rectilignes. Nous appliquons l'approximation eikonale dynamique à l'étude de réactions impliquant trois noyaux à halo différents : le $^{11}$Be, le $^{19}$C et le $^{8}$B. Pour les trois systèmes étudiés, nous confrontons nos résultats théoriques avec les données expérimentales disponibles. Nous constatons un très bon accord tant sur l'allure que sur l'ordre de grandeur des différentes sections efficaces. Ceci est valable aussi bien pour les collisions sur cible lourde que sur cible légère. Les motifs d'interférence présents dans les distributions angulaires sont également bien reproduits par notre modèle, y compris pour la diffusion élastique. Nous analysons la section efficace de dissociation expérimentale du $^{19}$C dans le but de déterminer la présence d'une résonance dans le spectre continu de ce noyau. Nous constatons que plusieurs options restent plausibles et que d'autres mesures sont nécessaires (sur cible légère, par exemple) pour confirmer nos hypothèses. La dissociation coulombienne du $^{8}$B fait l'objet de nombreuses études expérimentales dans le but d'obtenir des informations sur la réaction inverse qu'est la capture radiative $^{7}$Be(p,$gamma$)$^{8}$B. En analysant cinq expériences pour lesquelles différentes observables ont été mesurées, nous examinons la validité des hypothèses qui permettent de faire un lien direct entre dissociation et capture radiative. Nous observons que l'extraction d'informations sur la capture radiative à partir de données de dissociation semble plus compliqué qu'initiallement prévu. Cependant les différentes mesures permettent de valider un modèle de structure du $^{8}$B qui peut servir au calcul de la section efficace de capture radiative. L'approximation eikonale dynamique constitue donc un outil performant qui permet d'analyser toutes les observables liées à la dissociation élastique d'un noyau à halo sur une cible lourde ou légère à des énergies incidentes de quelques dizaines de MeV par nucléon.

This thesis examines factors, which influence responses on “paper and pencil” evaluations, commonly used with training programmes. A series of ten studies investigated evaluations of a wide range of courses, some taught by the researcher. It was emphasised, evaluations should take into account the educational variables of type of training, type of student and course content. Open ended evaluations were found to be influenced by a desire to react in a socially desirable manner. This interpretation was supported by student's responses on a questionnaire. The value of open ended evaluations as a probing mechanism was emphasised. Activity measure evaluations were found to relate more closely to the effort involved in the task than the to merits of a particular aspect of a course. Likert style structured rating scales were subject to a ‘halo effect'. Students also tended to answer using the favourable end of scales regardless of their real feelings. Combining two evaluation techniques was found to have a dramatic effect on response rate on open ended evaluations and thus validity. In addition response patterns produced conflicting findings between open ended and Likert style scales.. It is suggested the way people complete evaluation forms is partly a reflection of the impact of a range of influences, not formerly linked by research methods texts to evaluation form. It was stressed the educational aims of any evaluation should be established before methods of evaluation are decided.