Based on a Ph.D. thesis in the Dept. of Meteorology, 1967. / Bibliography: p. 99-101.

Thesis (M.S.)--University of Delaware, 2007. / Principal faculty advisor: Fabrice Veron, College of Marine and Earth Studies. Includes bibliographical references.

Thesis (M.Eng.)--Memorial University of Newfoundland, 2005. / Bibliography: leaves 71-76.

Thesis (Ph. D.)--University of Rhode Island, 2006. / Typescript. Includes bibliographical references (leaves 94-101).

Les émissions ultraviolettes des atmosphères de Vénus et de Mars, couramment appelées airglows, sont des phénomènes lumineux qui proviennent de relaxations d'atomes et de molécules passant d'un état excité à un état d'énergie inférieure. Ceux-ci nous renseignent sur les densités des constituants intervenant dans les réactions chimiques des atmosphères, ainsi que sur la dynamique des mésosphères respectives. Cette thèse traite de l'analyse détaillée de ces phénomènes dont le signal a été détecté entre 118 et 320 nm par les instruments SPICAV et SPICAM à bord des satellites Venus Express et Mars Express. Afin de bien comprendre le sujet abordé, les deux planètes, les différents airglows analysés et les instruments sont abordés dans une introduction constituant le premier chapitre de ce travail. Le chapitre 2 est consacré aux outils numériques qui servent à l'analyse et à la modélisation des airglows. Les trois chapitres suivants sont dédiés à leur caractérisation en intensité, à leur répartition en altitude et à leur localisation statistique. En particulier, nous étudions dans le chapitre 3 l'airglow de la molécule NO présent dans l'atmosphère nocturne de Mars à l'aide des données provenant de l'instrument SPICAM. Dans ce chapitre, nous utilisons un modèle chimique et diffusif unidimensionnel afin de confronter la théorie aux observations. Dans le chapitre 4, la même émission provenant de l'atmosphère de Vénus est analysée à l'aide du modèle unidimensionnel et des données enregistrées par l'instrument SPICAV. Les émissions de CO Cameron et du doublet CO2+ de l'atmosphère éclairée de Mars sont abordées dans le chapitre 5 à l'aide des données SPICAM. Ces émissions sont également comparées à un modèle stochastique afin de quantifier leurs processus de formation. Le chapitre 6 expose quelques perspectives de travail qui concernent ces phénomènes et qui permettrons à l'avenir d'acquérir de nouvelles informations à partir des données récoltées par SPICAV et SPICAM. Finalement, nous concluons en rassemblant les résultats clés des trois chapitres formant le corps principal de cette thèse.

In what atmosphere do people feel welcomed and comfortable? What are their needs, preferences, expectations and how do these affect their shopping behaviour? The proportion of older persons in the population is constantly growing so in the new future there will be more and more older shoppers in the stores. This study has from a management perspective tried to find a suitable store design and atmosphere that would be appreciated by the older shoppers segment. The research question of the study was: What store atmosphere and store design lead the growing target group - the elderly towards a sales increasing shopping behaviour? In attempt of answering the research question the main purpose was to understand the needs and preferences of older consumers and their shopping behaviour related to the issues of food shopping in a supermarket and to be able to discover underlying mechanisms in order to suggest a store atmosphere and store design adapted to the older consumers; and thus an increasing sales strategy for the store. In order to form a theoretical frame various secondary sources have been used that were found to be suitable for the research area. The retail anthropologist Paco Underhill has been a great inspiration for many theories in the study. Two qualitative methods have been used: structural observations and semi-structural interviews. The qualitative method is well chosen and makes it possible to fulfil the purpose of the study. Seven individuals were first observed in a store while shopping and later interviewed about their shopping experience. In the analysis the empirical data was analysed with some references drawn to the theoretical frame. Similar behavioural patterns were identified among the participants that formed the concepts: morning shoppers, one stop store, personal atmosphere, brand unawareness and finally service access. In conclusions a store strategy, based on older consumers needs and preferences, was proposed that would make the older consumers of the study feel more welcomed in the store and hence hopefully shop more. The strategy contained features like: more staff members in the morning, more efficient use of the in-store kitchen, development of “We Care” strategy and others. Researcher’s own reflections and suggestions as well as the veracity conclude this bachelor thesis.

Carbon Monoxide (CO) was discovered in the stratosphere of Neptune from the detection of the J=3-2 and J=2-1 rotational transitions in emission at 345.8 and 230.5 GHz respectively. It was conventionally thought that all of the atmospheric carbon should be in its reduced form of methane (CH₄). Two sources of stratospheric CO have been postulated: CO transported from the interior by convection due to Neptune's strong internal heat source (internal source); or, CO produced through photochemical reactions from an external supply of water (external source). <p>In this research project the J=3-2 transition of CO was observed to find the CO profile in Neptune's atmosphere and determine the mechanism producing CO. Three instruments were used at the James Clerk Maxwell Telescope (JCMT) to measure the CO line: the heterodyne receiver B3; the University of Lethbridge Fourier Transform Spectrometer (FTS); and, the Submillimeter Common User Bolometer Array (SCUBA). <p>The high resolution (1.25 MHz) of the heterodyne observations over a large frequency range (~20 GHz) produced a very powerful result because the narrow emission core from the stratosphere and the broad absorption feature arising in the lower atmosphere were measured simultaneously. The CO abundance profile was determined using a model of the J=3-2 CO transition in Neptune's atmosphere developed for this project. Calculations indicate a CO abundance of 1.9^+0.5_-0.3x10^-6 in the upper stratosphere and (0.8±0.2)x10^-6 in the lower stratosphere and troposphere. <p>The moderate resolution of the FTS data allowed the broad absorption feature to be measured. Uranus was originally chosen as the calibration source, but the discovery of CO in Uranus by Encrenaz et al. (2004), while this project was in progress, prompted both Neptune and Uranus to be examined for CO absorption. Two data sets (1993 and 2002) were analyzed and it was found that the 1993 spectra produced superior results, giving a CO mole ratio in the lower atmosphere between 0.8x10^-6 and 2x10^-5; this agrees, within the uncertainty limit, with the lower atmosphere heterodyne result. A tentative detection of CO in Uranus was also obtained from the 1993 data, with a CO abundance profile constrained to pressures greater than 0.5 bar with an abundance between 5x10^-7 and 1x10^-5. The 2002 data were found to be inferior to the 1993 data because of imperfect cancellation of thermal emission from the terrestrial atmosphere. <p> The 850ìm SCUBA filter profile is well matched to the width of the CO feature. Photometric observations of Neptune and Uranus were used to determine if the reduction in integrated flux due to CO absorption could be detected using SCUBA. A CO mole ratio in the range (1.2-1.7) x10^-6 was found for Neptune, calibrated against Uranus and assuming no CO in Uranus. Calibration of the Neptune and Uranus SCUBA data against Mars to produce an independent estimate of the CO abundance in both planets did not produce a useful result because of large calibration errors. <p>Comparison of the results from the three techniques determined that the heterodyne measurement was superior and the derived CO profile was used to determine the source of neptunian CO. It was concluded that the source of CO in Neptune is both internal and external. The lower atmosphere result indicates an interior dominated by water ice. The most likely mechanism for the upper atmosphere CO involves meteoritic ablation, photolysis of H₂O, and chemical reaction with by-products of methane photochemistry. The required H₂O influx for this mechanism is at least two orders of magnitude higher than previously observed, indicating either that the observed H₂O abundance is too small or that CO is produced by a different mechanism.

The Atmospheric Chemistry Experiment (ACE) is a satellite mission for remote sensing of the Earth's atmosphere using the solar occultation technique. The primary instrument on this satellite is the Atmospheric Chemistry Experiment Fourier Transform Spectrometer (ACE-FTS). ACE-FTS retrievals are described with a focus on the creation of <em>a priori</em> temperature and pressure profiles. ACE-FTS measurements are then used to investigate the chemistry, transport and trends of chlorine, fluorine and water in the stratosphere, leading to an improved understanding of processes affecting both stratospheric ozone depletion and global climate change. <br /><br /> Total chlorine (Cl_TOT) in the stratosphere is determined using ACE-FTS measurements of eleven chlorine-containing species, supplemented by both other measurements and models, to determine Cl_TOT as a function of altitude in five latitude zones. All resulting Cl_TOT profiles are nearly linear, with a slight slope. Mean Cl_TOT for 2004 is determined to be 3. 65 ppbv for both the northern and southern midlatitudes (with a precision and estimated accuracy of ±0. 09 and ±0. 13 ppbv, respectively). A slightly lower value of mean Cl_TOT is determined for the tropics and slightly higher values at high latitudes. Total fluorine (F_TOT) in the stratosphere is also determined primarily from ACE-FTS measurements using a similar approach, resulting in stratospheric F_TOT profiles which are nearly linear with mean values ranging from 2. 50 to 2. 59 ppbv for each latitude zone (with a precision of 0. 04-0. 07 ppbv and an estimated accuracy of 0. 15 ppbv). The observed slopes and pattern of latitudinal variation are evidence of the beginning of a decline in global stratospheric chlorine and of the continuing increase in global stratospheric fluorine levels. <br /><br /> The abundance of water in the stratosphere is investigated for the northern hemisphere midlatitudes in 2004 using ACE-FTS measurements. Potential water is determined as [H₂O]+2[CH₄] and from [H₂O] versus [CH₄] correlations, resulting in a value of 7. 14±0. 05 ppmv, which is used to determine a value of 3. 65±0. 15 ppmv for the mean abundance of water entering the stratosphere. Both values are compared directly with historical data from the Atmospheric Trace Molecule Spectroscopy (ATMOS) instrument (1985-1994) and show a negligible change, implying that the increases observed by ATMOS and other long-term measurements from that time period have not continued. <br /><br /> The removal of stratospheric water in the Arctic vortex is investigated using ACE-FTS measurements. Using derived quantities from a meteorological data assimilation, northern hemisphere occultations from early 2004 are classified as vortex, vortex edge or extravortex. [CH₄] versus [N₂O] correlations are used to further classify the extravortex occultations as tropical, subtropical or midlatitude. Comparisons between profiles of [N₂O], [CH₄] and [H₂O] inside and outside the Arctic vortex, give estimates of upper stratospheric and lower mesospheric descent rates, indicating that descent in the winter 2004 Arctic vortex was rapid, with evidence of descent at higher altitudes than in past years. <br /><br /> The dehydration of air in the tropical tropopause layer and mechanisms for the entry of water vapor into the stratosphere are investigated by an analysis of ACE-FTS profiles of temperature, water vapor and [HDO]/[H₂O]. Month-to-month comparisons for 2004 and 2005 reveal a clear pattern of seasonal variation and a correlation between minimum temperature and maximum HDO depletion. Further interpretation indicates that the gradual dehydration mechanism accompanied by lofting of ice particles in the tropical troposphere is the most likely explanation for the observed seasonal variation and the shape of the [HDO]/[H₂O] profiles.

Carbon Monoxide (CO) was discovered in the stratosphere of Neptune from the detection of the J=3-2 and J=2-1 rotational transitions in emission at 345.8 and 230.5 GHz respectively. It was conventionally thought that all of the atmospheric carbon should be in its reduced form of methane (CH₄). Two sources of stratospheric CO have been postulated: CO transported from the interior by convection due to Neptune's strong internal heat source (internal source); or, CO produced through photochemical reactions from an external supply of water (external source). <p>In this research project the J=3-2 transition of CO was observed to find the CO profile in Neptune's atmosphere and determine the mechanism producing CO. Three instruments were used at the James Clerk Maxwell Telescope (JCMT) to measure the CO line: the heterodyne receiver B3; the University of Lethbridge Fourier Transform Spectrometer (FTS); and, the Submillimeter Common User Bolometer Array (SCUBA). <p>The high resolution (1.25 MHz) of the heterodyne observations over a large frequency range (~20 GHz) produced a very powerful result because the narrow emission core from the stratosphere and the broad absorption feature arising in the lower atmosphere were measured simultaneously. The CO abundance profile was determined using a model of the J=3-2 CO transition in Neptune's atmosphere developed for this project. Calculations indicate a CO abundance of 1.9^+0.5_-0.3x10^-6 in the upper stratosphere and (0.8±0.2)x10^-6 in the lower stratosphere and troposphere. <p>The moderate resolution of the FTS data allowed the broad absorption feature to be measured. Uranus was originally chosen as the calibration source, but the discovery of CO in Uranus by Encrenaz et al. (2004), while this project was in progress, prompted both Neptune and Uranus to be examined for CO absorption. Two data sets (1993 and 2002) were analyzed and it was found that the 1993 spectra produced superior results, giving a CO mole ratio in the lower atmosphere between 0.8x10^-6 and 2x10^-5; this agrees, within the uncertainty limit, with the lower atmosphere heterodyne result. A tentative detection of CO in Uranus was also obtained from the 1993 data, with a CO abundance profile constrained to pressures greater than 0.5 bar with an abundance between 5x10^-7 and 1x10^-5. The 2002 data were found to be inferior to the 1993 data because of imperfect cancellation of thermal emission from the terrestrial atmosphere. <p> The 850ìm SCUBA filter profile is well matched to the width of the CO feature. Photometric observations of Neptune and Uranus were used to determine if the reduction in integrated flux due to CO absorption could be detected using SCUBA. A CO mole ratio in the range (1.2-1.7) x10^-6 was found for Neptune, calibrated against Uranus and assuming no CO in Uranus. Calibration of the Neptune and Uranus SCUBA data against Mars to produce an independent estimate of the CO abundance in both planets did not produce a useful result because of large calibration errors. <p>Comparison of the results from the three techniques determined that the heterodyne measurement was superior and the derived CO profile was used to determine the source of neptunian CO. It was concluded that the source of CO in Neptune is both internal and external. The lower atmosphere result indicates an interior dominated by water ice. The most likely mechanism for the upper atmosphere CO involves meteoritic ablation, photolysis of H₂O, and chemical reaction with by-products of methane photochemistry. The required H₂O influx for this mechanism is at least two orders of magnitude higher than previously observed, indicating either that the observed H₂O abundance is too small or that CO is produced by a different mechanism.

It has been argued that a secure and comfortable atmosphere is essential in order for a therapeutic or learning environment to be beneficial (Bakken 1998). In Functionally Oriented Music Therapy (FMT) there are arguably certain elements that help create this kind of atmosphere. By looking at the nature of FMT, what these elements might be, and FMT with two different clients, this paper tries to obtain a clearer idea of what creates a secure and comfortable atmosphere in FMT.