The effect of frontal features on chlorophyll concentration within the Kuroshio

Senior thesis written for Oceanography 445

The effect of shore armoring on beach slope in mixed sand-and-gravel beaches

Senior thesis written for Oceanography 445

Climatology of the Iberia coastal low-level wind jet: weather research forecasting model high-resolution results

Coastal low-level jets (CLLJ) are a low-tropospheric wind feature driven by the pressure gradient produced by a sharp contrast between high temperatures over land and lower temperatures over the sea. This contrast between the cold ocean and the warm land in the summer is intensified by the impact of the coastal parallel winds on the ocean generating upwelling currents, sharpening the temperature gradient close to the coast and giving rise to strong baroclinic structures at the coast. During summertime, the Iberian Peninsula is often under the effect of the Azores High and of a thermal low pressure system inland, leading to a seasonal wind, in the west coast, called the Nortada (northerly wind). This study presents a regional climatology of the CLLJ off the west coast of the Iberian Peninsula, based on a 9km resolution downscaling dataset, produced using the Weather Research and Forecasting (WRF) mesoscale model, forced by 19 years of ERA-Interim reanalysis (1989-2007). The simulation results show that the jet hourly frequency of occurrence in the summer is above 30% and decreases to about 10% during spring and autumn. The monthly frequencies of occurrence can reach higher values, around 40% in summer months, and reveal large inter-annual variability in all three seasons. In the summer, at a daily base, the CLLJ is present in almost 70% of the days. The CLLJ wind direction is mostly from north-northeasterly and occurs more persistently in three areas where the interaction of the jet flow with local capes and headlands is more pronounced. The coastal jets in this area occur at heights between 300 and 400 m, and its speed has a mean around 15 m/s, reaching maximum speeds of 25 m/s.

Wind resource modelling in complex terrain using different mesoscale–microscale coupling techniques

Wind resource evaluation in two sites located in Portugal was performed using the mesoscale modelling system Weather Research and Forecasting (WRF) and the wind resource analysis tool commonly used within the wind power industry, the Wind Atlas Analysis and Application Program (WAsP) microscale model. Wind measurement campaigns were conducted in the selected sites, allowing for a comparison between in situ measurements and simulated wind, in terms of flow characteristics and energy yields estimates. Three different methodologies were tested, aiming to provide an overview of the benefits and limitations of these methodologies for wind resource estimation. In the first methodology the mesoscale model acts like “virtual” wind measuring stations, where wind data was computed by WRF for both sites and inserted directly as input in WAsP. In the second approach, the same procedure was followed but here the terrain influences induced by the mesoscale model low resolution terrain data were removed from the simulated wind data. In the third methodology, the simulated wind data is extracted at the top of the planetary boundary layer height for both sites, aiming to assess if the use of geostrophic winds (which, by definition, are not influenced by the local terrain) can bring any improvement in the models performance. The obtained results for the abovementioned methodologies were compared with those resulting from in situ measurements, in terms of mean wind speed, Weibull probability density function parameters and production estimates, considering the installation of one wind turbine in each site. Results showed that the second tested approach is the one that produces values closest to the measured ones, and fairly acceptable deviations were found using this coupling technique in terms of estimated annual production. However, mesoscale output should not be used directly in wind farm sitting projects, mainly due to the mesoscale model terrain data poor resolution. Instead, the use of mesoscale output in microscale models should be seen as a valid alternative to in situ data mainly for preliminary wind resource assessments, although the application of mesoscale and microscale coupling in areas with complex topography should be done with extreme caution.

Impact of the Meteorology Conditions on the Particulate Matter Dispersion from an Industrial Complex into Urban and Suburban Areas

The aim of this work was to assess the influence of meteorological conditions on the dispersion of particulate matter from an industrial zone into urban and suburban areas. The particulate matter concentration was related to the most important meteorological variables such as wind direction, velocity and frequency. A coal-fired power plant was considered to be the main emission source with two stacks of 225 m height. A middle point between the two stacks was taken as the centre of two concentric circles with 6 and 20 km radius delimiting the sampling area. About 40 sampling collectors were placed within this area. Meteorological data was obtained from a portable meteorological station placed at approximately 1.7 km to SE from the stacks. Additional data was obtained from the electrical company that runs the coal power plant. These data covers the years from 2006 to the present. A detailed statistical analysis was performed to identify the most frequent meteorological conditions concerning mainly wind speed and direction. This analysis revealed that the most frequent wind blows from Northwest and North and the strongest winds blow from Northwest. Particulate matter deposition was obtained in two sampling campaigns carried out in summer and in spring. For the first campaign the monthly average flux deposition was 1.90 g/m2 and for the second campaign this value was 0.79 g/m2. Wind dispersion occurred predominantly from North to South, away from the nearest residential area, located at about 6 km to Northwest from the stacks. Nevertheless, the higher deposition fluxes occurred in the NW/N and NE/E quadrants. This study was conducted considering only the contribution of particulate matter from coal combustion, however, others sources may be present as well, such as road traffic. Additional chemical analyses and microanalysis are needed to identify the source linkage to flux deposition levels.

Fate Hazardous elements in soils surrounding a coal-fired power plant complex

Proceedings of the 13th International UFZ-Deltares Conference on Sustainable Use and Management of Soil, Sediment and Water Resources - 9–12 June 2015 • Copenhagen, Denmark

Influência dos equipamentos de aquecimento, arrefecimento e AQS na certificação energética de edifícios

Na União Europeia os sectores dos transportes e da indústria são ambos grandes consumidores de energia, mas são os edifícios residenciais e de serviços onde o consumo energético é maior, e em 2005, segundo a EnerBuilding, representavam cerca de 17% dos consumos de energia primária em termos nacionais. A energia gasta com a iluminação, o aquecimento, o arrefecimento e AQS das habitações, locais de trabalho e locais de lazer é superior à consumida pelos sectores dos transportes e da indústria. As habitações representam dois terços do consumo total de energia dos edifícios europeus, o qual aumenta todos os anos com a melhoria da qualidade de vida, traduzindo-se numa maior utilização dos sistemas de climatização. Neste sentido, e de acordo com o decreto-lei que transpõe para a legislação portuguesa a diretiva comunitária relativa ao desempenho energético dos edifícios, todos os Estados da União Europeia devem ter um sistema de certificação energética para informar o cidadão sobre a qualidade térmica dos edifícios, aquando da construção, da venda ou do arrendamento. Assim, entrou em vigor em Portugal, desde 1 de Janeiro de 2009, a obrigatoriedade de apresentação de um certificado de eficiência energética, no ato de compra, venda ou aluguer de edifícios novos e existentes. A certificação energética permite assim aos futuros utilizadores dos edifícios obter informação sobre os potenciais consumos de energia, no caso dos novos edifícios ou no caso de edifícios existentes sujeitos a grandes intervenções de reabilitação, dos seus consumos reais ou aferidos para padrões de utilização típicos, passando o consumo energético a integrar um conjunto dos aspetos importantes para a caracterização de qualquer edifício. Em edifícios de serviços, o certificado energético assegura aos utentes do edifício ou da fração que este reúne condições para garantir a eficiência energética e a adequada qualidade do ar interior. Uma vez que passamos 80% do nosso tempo em edifícios, e que isto se reflete num consumo cada vez mais elevado do sector residencial e dos serviços no consumo total energético do país, este trabalho pretende fazer a comparação dos vários equipamentos de aquecimento, de arrefecimento e de AQS e qual a influência dos mesmos na certificação energética de edifícios, e consequentemente na eficiência dos mesmos, sendo que a eficiência e a certificação energética de um edifício deve ser um aspeto relevante a levar em consideração no momento do planeamento ou da construção, bem como na aquisição de uma nova habitação. Um projeto concebido de modo a tirar proveito das condições climáticas, da orientação solar, dos ventos dominantes e utilizadas técnicas construtivas e os materiais adequados, é possível reduzir os gastos energéticos com a iluminação ou os sistemas de climatização.

Pollen and grain size records in abyssal sediments of the northwest Pacific Ocean as proxies of Plio-Pleistocene climate change /

A distinctive period of global change occurred during the PUocene between the warm Miocene and subsequent Quaternary cooling. Samples from Ocean Drilling Project Site 11 79 (-5586 mbsl, 41°4'N, 159°57'E), Site 881 (-5765 mbsl, 47°6.133'N, 161°29.490'E) and Site 882 (-3255 mbsl, 50°22'N, 167°36'E) were studied to determine the magnitude and composition ofterrigenous flux to the western mid-latitude North Pacific and its relation to climate change in East Asia since the mid-Pliocene. Dust-sized particles (including pollen), sourced from the arid regions and loess plateaus in East Asia are entrained by prevailing westerly winds and transported to the midlatitude northwest North Pacific Ocean. This is recorded by peaks in the total concentration of pollen and spores, as well as the mean grain size of allochthonous and autochthonous silicate material in abyssal marine sediments. Aridification of the Asian interior due to the phased uplift of the Himalayan-Tibetan Plateau created the modem East Asian Monsoon system dominated by a strengthening of the winter monsoon. The winter monsoon is further enhanced during glacials due to the expansion of desert and steppe environments at the expense ofwoodlands and forests recorded by the composition of palynological assemblages. The late Pliocene-Pleistocene glacials at ODP Sites 1 179, 881, and 882 are characterized by increases in grain size, magnetic susceptibility, pollen and spore concentrations around 3.5-3.3, 2.6-2.4, 1.7-1.6, and 0.9-0.7 Ma (ages based on magnetostratigraphic and biostratigraphic datums). The peaks during these times are relatively rich in pollen taxa derived primarily from steppe and boreal vegetation zones, recording cool, dry climates. The overall size increase of sediment and abundance of terrestrial palynomorphs record enhanced wind strength. The increase in magnitude of pollen and spore concentrations as well as grain size record global cooling and Northern Hemisphere glaciation. The peaks in grain size as well as pollen and spore abundance in marine sediments correlate with the mean grain size of loess in East Asia, consistent with the deflation of unarmoured surfaces during glacials. The transport of limiting nutrients to marine environments enhanced sea surface productivity and increased the rate of sediment accumulation.

View of Falls from Steel Bridge, Niagara, U.S.A.

The description of the image reads "(4)-8972-General view of Falls from new steel bridge - Maid of the Mist at landing - Niagara, U.S.A." The reverse of the image includes the description, "We are standing on the new steel bridge over Niagara River, 190 feet above the water and looking a little west of south, up the river towards Lake Erie. The high cliff at the extreme left, on the American side, is Prospect Point, where a crowd is gathered at this moment to view the Falls that we see just beyond Prospect Point. That dark, tree-covered mass of rock beyond is Goat Island; and just this side of Goat Island we see a bit of its precipice has been cut off separate from the rest by the powerful current of the waters - the smaller portion is Luna Island, and the Luna Falls go pouring down between the two islands. The face of the precipice curves inward beneath the Luna Falls leaving behind the 160 foot sheet of water the unearthly hollow known as the Cave of the Winds. Beyond Goat Island we see the gigantic curve of the Horseshoe Falls, 3,010 feet long and 158 feet high, reaching around through the clouds of spray to the farther Canadian shore. (The boundary line between British and American territory is in mid-stream.) It has been estimated that every minute 375,000 tons of water pour over these Horseshoe Falls, and they are wearing away the cliffs, moving back up the stream at the rate of 2.4 feet per year. It was probably only about a thousand years ago that they took their plunge just about where we stand now. Down there below us, at the wharf is the Maid of the Mist at the American landing taking on passengers who have come down the steep bank by the inclined railway. Its course takes it through those clouds of spray almost to the very foot of both Falls, - waters falling from 167 feet overhead, and water surging at least as many feet deep under the staunch little vessel. See special 'keyed' maps of Niagara pub. by Underwood and Underwood, also the Niagara Book by Mark Twain, W.D. Howells and others."

Niagara Falls Handbill Collection, 1838-1886, n.d. (non-inclusive)

According to legend, the Burning Springs were discovered by early natives in the Niagara Peninsula. Bridgewater Mills was built on the site of the spring. During the excavation of the factory; workmen uncovered the spring. Samuel Street and Thomas Clark recognized the potential of this as a tourist attraction so they built a wooden shelter over the spring. The spring was covered with a barrel with a pipe protruding from it. This became the first tourist attraction at Niagara. The Cave of the Winds was a cavern located behind the Bridal Veil Fall. It was originally named the Aeolus Cave. In 1920, a sudden rock fall from the ceiling killed 3 tourists. The cave was destroyed in 1955 as it was deemed dangerous. The captain of the Maid of the Mist was usually a farmer who owned the land where the ship docked. In 1846, the first steam powered Maid of the Mist was launched. By 1848, the first suspension bridge was built over the gorge and the main purpose of the Maid of the Mist was no longer to carry people who needed to travel, but now the focus was on people who wanted to view the Falls at close range. Source: http://www.niagarafrontier.com/burningsprings.html http://www.niagarafrontier.com/winds.html http://reservationsystems.com/niagara_daredevils/maid_of_the_mist.html

La composition au moyen des quarts de ton

La version intégrale de cette thèse est disponible uniquement pour consultation individuelle à la Bibliothèque de musique de l’Université de Montréal.

Étude du système binaire CV Ser à l'aide du satellite MOST

Ce mémoire s’intéresse au système binaire massif CV Serpentis, composé d’une Wolf- Rayet riche en carbone et d’une étoile de la séquence principale, de type spectral O (WC8d + O8-9IV). D’abord, certains phénomènes affectant les étoiles massives sont mentionnés, de leur passage sur la séquence principale à leur mort (supernova). Au cours du premier cha- pitre, un rappel est fait concernant certaines bases de l’astrophysique stellaire observa- tionnelle (diagramme Hertzsprung-Russell, phases évolutives, etc...). Au chapitre suivant, un des aspects les plus importants de la vie des étoiles massives est abordé : la perte de masse sous forme de vents stellaires. Un historique de la découverte des vents ouvre le chapitre, suivi des fondements théoriques permettant d’expliquer ce phénomène. Ensuite, différents aspects propres aux vents stellaires sont présentés. Au troisième chapitre, un historique détaillé de CV Ser est présenté en guise d’introduc- tion à cet objet singulier. Ses principales caractéristiques connues y sont mentionnées. Finalement, le cœur de ce mémoire se retrouve au chapitre 4. Des courbes de lumière ultra précises du satellite MOST (2009 et 2010) montrent une variation apparente du taux de perte de masse de la WR de l’ordre de 62% sur une période orbitale de 29.701 jours. L’analyse des résidus permet de trouver une signature suggérant la présence de régions d’interaction en corotation (en anglais corotating interaction regions, ou CIR) dans le vent WR. Une nouvelle solution orbitale est présentée ainsi que les paramètres de la région de collision des vents et les types spectraux sont confirmés.

Étude observationnelle de la collision des vents dans les systèmes Wolf-Rayet+O

Nous présentons les résultats de trois campagnes d'observation d'un mois chacune dans le cadre de l'étude de la collision des vents dans les systèmes binaires Wolf-Rayet + OB. Ce travail se concentre sur l'étude des objets de l'hémisphère sud n'ayant jamais encore fait l'objet d'études poussées dans ce contexte. À cela, nous avons ajouté l'objet archétype pour ce type de systèmes : WR 140 (WC7pd + O5.5fc) qui a effectué son dernier passage périastre en janvier 2009. Les deux premières campagnes (spectroscopiques), ont permis une mise à jour des éléments orbitaux ainsi qu'une estimation de la géométrie de la zone de collision des vents et d'autres paramètres fondamentaux des étoiles pour 6 systèmes binaires : WR 12 (WN8h), 21 (WN5o+O7V), 30 (WC6+O7.5V), 31 (WN4o+O8), 47 (WN6o+O5) et 140. Une période non-orbitale courte (probablement reliée à la rotation) a également été mesurée pour un des objets : WR 69 (WC9d+OB), avec une période orbitale bien plus grande. La troisième campagne (photométrique) a révélé une variabilité étonnamment faible dans un échantillon de 20 étoiles WC8/9. Cela supporte l'idée que les pulsations ne sont pas courantes dans ce type d'étoiles et qu'il est peu probable que celles-ci soient le mécanisme dominant de formation de poussière, suggérant, par défaut, le rôle prédominant de la collision des vents.

Étude de la variabilité spectroscopique d’un échantillon d’étoiles Wolf-Rayet de type WC9

Nous savons que la grande majorité des étoiles WC9 produit de la poussière à base de carbone. Cette dernière doit se former dans des zones de très haute densité afin de survivre à l’environnement hostile qu’est celui du vent d’une étoile WR. Les étoiles WC appartenant à un système binaire WR + O produisent de la poussière quand les vents des deux étoiles entrent en collision et forment une zone de choc pouvant augmenter la densité du gaz d’un facteur 1000. Par contre, plusieurs étoiles WC9 n’ont, à ce jour, montré aucun signe de la présence d’un compagnon. Le but du projet est de tenter d’identifier un mécanisme alternatif responsable de la formation de poussière dans les étoiles WC9 n’appartenant pas à un système binaire. Nous présentons les résultats d’une campagne d’observation visant à caractériser la variabilité spectroscopique d’un échantillon de huit étoiles WC9 et une étoile WC8d. Nos résultats indiquent que la majorité des étoiles montrent des variations à grande échelle dans la raie d’émission C III 5696, soit à un niveau d’au moins 5% du flux de la raie et que les structures dans le vent ont une dispersion de vitesses de l’ordre de 150-300 km/s. De manière générale, les variations de vitesse radiales sont anti-corrélées avec le coefficient d’asymétrie de la raie, ce qui semble infirmer la présence d’un compagnon. Des observations en photométrie de l’étoile WR103 montrent une période de 9.1 ± 0.6 jours qui s’accorde avec les variations spectroscopiques et qui ne semble pas, de manière évidente, d’origine binaire.

Recherche de champs magnétiques chez les étoiles Wolf-Rayet par l'analyse d'observations spectropolarimétriques.

Cette thèse de doctorat présente les résultats d'un relevé spectropolarimétrique visant la détection directe de champs magnétiques dans le vent d'étoiles Wolf-Rayet (WR). Les observations furent entièrement obtenues à partir du spectropolarimètre ESPaDOnS, installé sur le télescope de l'observatoire Canada-France-Hawaii. Ce projet débuta par l'observation d'un étoile très variable de type WN4 appelée EZ CMa = WR6 = HD 50896 et se poursuivit par l'observation de 11 autres étoiles WR de notre galaxie. La méthode analytique utilisée dans cette étude vise à examiner les spectres de polarisation circulaire (Stokes V) et à identifier, au travers des raies d'émission, les signatures spectrales engendrées par la présence de champs magnétiques de type split monopole dans les vents des étoiles observées. Afin de pallier à la présence de polarisation linéaire dans les données de polarisation circulaire, le cross-talk entre les spectres Stokes Q et U et le spectre Stokes V fut modélisé et éliminé avant de procéder à l'analyse magnétique. En somme, aucun champ magnétique n'est détecté de manière significative dans les 12 étoiles observées. Toutefois, une détection marginale est signalée pour les étoiles WR134, WR137 et WR138 puisque quelques-unes de leur raies spectrales semblent indiquer la présence d'une signature magnétique. Pour chacune de ces trois étoiles, la valeur la plus probable du champ magnétique présent dans le vent stellaire est respectivement de B ~ 200, 130 et 80 G. En ce qui concerne les autres étoiles pour lesquelles aucune détection magnétique ne fut obtenue, la limite supérieure moyenne de l'intensité du champ qui pourrait être présent dans les données, sans toutefois être détecté, est évaluée à 500 G. Finalement, les résultats de cette étude ne peuvent confirmer l'origine magnétique des régions d'interaction en co-rotation (CIR) observées chez plusieurs étoiles WR. En effet, aucun champ magnétique n'est détecté de façon convaincante chez les quatre étoiles pour lesquelles la présence de CIR est soupçonnée.