Ground level ozone is one of the most ubiquitous air pollutants in urban areas, and is generated by photochemical reactions of oxides of nitrogen (NOx) and volatile organic compounds (VOCs). The effectiveness of emission reduction strategies for ozone precursors is typically evaluated using gridded, photochemical air quality models. One of the underlying assumptions in these models is that industrial emissions are nearly constant, since many industrial facilities operate continuously at a constant rate of output. However, recent studies performed in the Houston-Galveston-Brazoria area indicate that some industrial emission sources exhibit high temporal emission variability that can lead to very rapid ozone formation, especially when emissions are composed of highly reactive volatile organic compounds. This work evaluates the impact of variable emissions from industrial sources on ground-level ozone formation in Houston area, utilizing a unique hourly emission inventory, known as the 2006 Special Inventory, created as a part of the second Texas Air Quality Study. Comparison of the hourly emissions inventory data with ambient measurements indicated that the impact of the variability of industrial source emissions on ozone can be significant. Photochemical modeling predictions showed that the variability in industrial emissions can lead to differences in local ozone concentrations of as much as 27 ppb at individual ozone monitor locations. The hourly emissions inventory revealed that industrial source emissions are highly variable in nature with diverse temporal patterns and stochastic behavior. Petrochemical and chemical manufacturing flares, which represent the majority of emissions in the 2006 Special Inventory, were grouped into categories based on industrial process, chemical composition of the flared gas, and the temporal patterns of their emissions. Stochastic models were developed for each categorization of flare emissions with the goal of simulating the characterized temporal emission variability. The stochastic models provide representative temporal profiles for flares in the petrochemical manufacturing and chemical manufacturing sectors, and as such serve as more comprehensive input for photochemical air quality modeling. / text

Made available in DSpace on 2016-03-15T19:35:53Z (GMT). No. of bitstreams: 1 Ray Fernando Hidalgo Ramirez.pdf: 3985319 bytes, checksum: 0a36b0e596cb2c3f1eadaccfa8f843ee (MD5) Previous issue date: 2015-06-17 / Universidade Presbiteriana Mackenzie / Solar flares radio emissions provide detailed information on the energy release, particle acceleration, heating processes and plasma conditions at the sites where the radiation is generated. This study focuses in radio emission from millimeter, sub-millimeter and another complementary wavelengths obtained by recent observations that might improve the understanding of processes from the low chromosphere to the corona. Here we study a GOES class X1.7 flare on January 27, 2012 detected by the Solar Sub-millimeter Telescope (SST) at 212 and 405 GHz, and by the solar radio polarimeters (POEMAS) at 45 and 90 GHz. LASCO C2 coronagraph observed a coronal mass ejection (CME) with possible physical connection with phenomena observed at radio-frequencies, including changes in polarization degree (45 and 90 GHz) and enhancements of scintillation index (212 and 405 GHz). The complementary radio observations were obtained by the Radio Solar Telescopes Network (RSTN) at the single frequencies 0.2, 0.4, 0.6, 1.4, 2.7, 4.9, 8.8 and 15.4 GHz and at the 25 - 180 MHz band, and by the Green Bank Solar Radio Burst Spectrometer (GBSRBS) at the 100 - 300 MHz and 300 - 1200 MHz bands. The solar flare exhibits a complex time structure at microwaves consisting of three major enhancements. Type III-like metric and decametric bursts were accompanied by small polarized burst at 45 and 90 GHz with polarization degrees of 0.09 and 0.12, suggesting changes in the magnetic field strength the order of 700 and 2000 G, respectively. SST detected one impulsive burst and significant 10% enhancements of scintillation index intermittently throughout the event. The CME launch time inferred by back extrapolation of the LASCO coronagraph observations to the solar limb coincides approximately in time to the changes in polarization degree, suggesting that CME might be a result of a magnetic transient causing an instability generating the subsequent impulsive structures. / As emissões em rádio das explosões solares provém informações detalhadas dos processos de liberação de energia, aceleração de partículas, aquecimento e condições do plasma na região onde a radiação é gerada. Este estudo concentra-se em rádio emissões nos comprimentos de onda milimétricos, sub-milimétricos e outras frequências complementares obtidas por observações recentes que podem melhorar o entendimento dos processos na baixa cromosfera até a coroa. Foi estudada uma explosão solar classe GOES X1.7 ocorrida no dia 27 de janeiro de 2012, detectada pelo Telescópio Solar Sub-milimétrico (SST) em 212 e 405 GHz e pelos rádio polarímetros solares em 45 e 90 GHz. Uma ejeção de massa coronal (CME) foi observada pelo coronógrafo C2 de LASCO com possível conexão física com os fenômenos observados em rádio frequências, incluindo mudanças no grau de polarização (45 e 90 GHz) e aumentos no índice de cintilação (212 e 405 GHz). As rádio observações complementares foram obtidas em frequências distintas, pela Rede de Rádio Telescópios Solares (RSTN), de 0,2; 0,4; 0,6; 1,4; 2,7; 4,9; 8,8 e 15,4 GHz e nas faixas de 25 - 180 MHz, e pelo Rádio Espectrômetro Solar Green Bank (GBSRBS) nas faixas de 100 - 300 MHz e 300 - 1200 MHz. A explosão solar apresenta uma estrutura temporal complexa em micro-ondas composta por três aumentos característicos. Explosões métricas e decamétricas tipo III foram acompanhadas por pequenas explosões com polarização em 45 e 90 GHz com graus de polarização de 0,09 e 0,12, sugerindo variações de campo magnético da ordem de 700 e 2000 G, respectivamente. O SST detectou uma explosão impulsiva e aumentos significativos de 10% no índice de cintilação de forma intermitente durante todo o evento. O tempo de lançamento da CME inferido por extrapolação das observações do coronógrafo LASCO ao limbo solar coincide aproximadamente com o instante do excesso de emissão e mudança do grau de polarização em 45 e 90 GHz, sugerindo que a CME tenha resultado de um transiente magnético ocasionando uma instabilidade que gerou as estruturas impulsivas subsequentes.

Made available in DSpace on 2016-03-15T19:35:55Z (GMT). No. of bitstreams: 1 Amauri Shossei Kudaka.pdf: 14809012 bytes, checksum: 1dc60260bb5dcd12adfa496880fb2a7e (MD5) Previous issue date: 2015-08-20 / High cadence solar observations in infrared and H-α are important tools for the study of active regions during solar flaring events. The acquisition and analysis of these observational data associated with information in other frequency bands, can be helpful in the study of emission mechanisms during solar flares. Recently it was installed at the Universidade Presbiteriana Mackenzie, São Paulo, the Mackenzie Solar Observatory, with the objective to provide research opportunities in Solar Physics. Experimental tests carried out in the Observatory should provide advances in instrumentation, assembly and procedures to be implemented and operated in collaboration with others observatories, for solar observations from ground and space. In this work, the physical structure of the Solar Observatory Mackenzie is described in details.Operating procedures of instruments and data acquisition are proposed, as well as the systematization of simultaneous observations at infrared and H-α. Despite the short time of operation, records of some solar events have already been obtained. / Observações solares em infravermelho e H-α, em alta cadência, são importantes ferramentas para o estudo de regiões ativas durante eventos solares explosivos. A obtenção e a análise destes dados observacionais, associados com informações em outras faixas do espectro, podem auxiliar no estudo dos mecanismos de emissão durante explosões solares. Recentemente foi instalado na Universidade Presbiteriana Mackenzie, São Paulo, o Observatório Solar Mackenzie, com o objetivo de fornecer oportunidades de pesquisa na área de Física Solar. Ensaios experimentais realizados no Observatório deverão proporcionar avanços na instrumentação, montagem e procedimentos a serem implementados e operados em colaboração com outros observatórios, para observações solares a partir do solo e do espaço. Neste trabalho, a estrutura física do Observatório Solar Mackenzie é descrita em detalhes. Procedimentos de operação dos instrumentos e de aquisição de dados são propostos, bem como a sistematização das observações simultâneas em infravermelho e H-α. Apesar do pouco tempo de operação, registros de vários eventos solares já foram obtidos.

This research focuses on measurements of a convective shear-layer instability seen naturally in quiet hypersonic flow. Experiments were carried out in the Boeing/AFOSR Mach 6 Quiet Tunnel (BAM6QT) at Purdue University. The BAM6QT provides low-disturbance hypersonic flow with freestream noise levels similar to what would be experienced by a flight vehicle. To obtain high-speed, off-the-surface measurements of the instability, a modified focused laser differential interferometer (FLDI) was first designed to work with the contoured Plexiglas windows available in the tunnel.<div><br>A cone-cylinder-flare geometry was then selected to study the instabilities related to an axisymmetric separation bubble at Mach 6. The sharp cone had a 5-degree half-angle, while flare angles of 10 degrees and 3.5 degrees were tested to compare axisymmetric compression with and without separation, respectively. Under quiet flow, laminar separation and reattachment was confirmed by schlieren and surface pressure-fluctuation measurements. Coherent traveling waves were observed. These were attributed to both the second-mode instability, as well as a shear-generated instability from the separation bubble. The symmetry of the bubble was found to be highly sensitive to angle of attack. Additionally, by introducing controlled disturbances on the cone upstream of the separation, larger-amplitude shear-generated waves were measured while the second-mode amplitudes remained unchanged. Therefore, the shear-generated waves were amplified moving through the shear layer, while the second mode remained neutrally stable. These appear to be the first measurements of traveling waves that are generated in the shear layer of a separation bubble in hypersonic flow. <br></div>

<p dir="ltr">Pressure transducer, infrared heat transfer, and schlieren imaging data for a flared cone and cone-cylinder-flare in Mach 6 quiet flow are presented. Flared cone pressure transducer results show second-mode RMS values comparable to that found in prior experimental work. Second-mode frequency is found to linearly increase with increasing freestream unit Reynolds number, and frequency varies little between sensors for a given freestream unit Reynolds number. Turbulent intermittency begins to increase at a freestream unit Reynolds number 2x10⁶/m greater than the unit Reynolds number corresponding to peak second-mode RMS. peak RMS. High-speed schlieren imaging on the downstream section of the flared cone shows the second-mode disturbance following trends in power which correlate with PCB RMS. Infrared heat transfer results contain the azimuthal heating streak pattern observed for the flared cone in prior research, but the hot-cold-hot streak pattern is not seen due to limited model length. Streak heating occurs downstream of second-mode peak RMS over the freestream unit Reynolds number range of 6.4x10⁶/m to 10.4x10⁶/m. The heat transfer of streaks is found to vary significantly from streak to streak, while mean streak heating variation with freestream unit Reynolds number is small.</p><p dir="ltr">PCB results of the cone-cylinder-flare show intermittent turbulence at a freestream unit Reynolds number of 16.0x10⁶/m. Examination of shear-layer and second-mode instabilities show significant increases in RMS moving downstream along the flare and with increasing freestream unit Reynolds number. High-speed schlieren imaging of the shear-layer reattachment region on the flare show the presence of the shear-layer and second-mode instabilities when the model is configured with a sharp nose tip. The instabilities are not present with a blunt 5 mm radius nose tip. Heat transfer is observed to increase along the downstream portion of the flare. The sharp nose tip configuration has higher heat transfer rates than the 5 mm radius nose tip configuration.</p>

Made available in DSpace on 2016-06-02T19:03:58Z (GMT). No. of bitstreams: 1 5593.pdf: 13078959 bytes, checksum: 1cc88a226e87c0a4ca26af32176acea5 (MD5) Previous issue date: 2013-08-19 / Financiadora de Estudos e Projetos / The requirements imposed by the new applications presents great challenges to the computation. There is not a perfect computer architecture, capable to attend to all the requirements. The parallel and hybrid computer arrangement rise as a solution to this scenario i.e., the CPU-Coprocessor pair arrangement can form a specialized computerized instrument for a special application task. This doctoral thesis proposes a parallel and hybrid computational platform denoted CoP-WS, that uses the interoperability technology known as Web Services. As coprocessor it is used the graphic processing unit, known as the GPU, functioning recently as parallel thread level processing of general use applications. The platform test of feasibility was inspired in radio astronomy, and it has been implemented two applications: a complex correlator of signals provided by a radio interferometric arrangement, and a flare recognition system with a solar radio interferometer image. Both processings can be inserted in the context of pipeline execution, using sufficient configuration of CPU-GPU pairs, having on one side the interferometric arrangement antenna signal input and in the other side the result of the solar flare recognition. The obtained results of the both applications show the feasibility of the CoP-WS platform, for greater volume of data being processed in quasi real time. In the case of the correlator the average processing time in each integration period was around 160 ms, and in the case of the solar flare recognition, 48 ms for each solar disk image. / Os requisitos impostos pelas novas aplicações, sejam estas científicas, ou não, apresentam grandes desafios à computação. Não existe uma arquitetura de computadores "perfeita" que seja capaz de atender a todos estes requisitos. A configuração de arranjos paralelos e híbridos de computadores se apresenta como uma solução para este cenário, ou seja, a configuração de arranjos de pares CPU-Coprocessador, pode ser especializada para o processamento de uma aplicação distintas. Este trabalho de doutorado propõe uma plataforma computacional paralela e híbrida distribuída denominada CoP-WS, que utiliza a tecnologia de interoperabilidade conhecida como Web Services. Como coprocessador é utilizada a unidade de processamento gráfico conhecida como GPU, cuja função tem sido de processamento paralelo ao nível de threads, para aplicações gerais nos últimos tempos. A prova de viabilidade da plataforma implementada foi inspirada na radioastronomia, tendo sido implementados dois aplicativos: um correlacionador complexo de sinais provindos dos arranjos interferométricos e um sistema para o reconhecimento de explosões solares, numa imagem de radiointerferometria solar. Ambos os processamentos podem ser inseridos num contexto de execução em pipeline, usando uma configuração suficiente de pares CPU-GPU, tendo de um lado a entrada dos sinais das antenas do arranjo interferométrico e do outro lado o resultado do processamento de reconhecimento de explosões solares. Em ambas aplicações os resultados foram satisfatórios sendo que no caso do correlacionador o tempo médio de processamento de cada ciclo de integração foi de aproximadamente 160 ms, e para a aplicação de reconhecimento de explosões solares, de 48 ms por imagem de disco solar.

[pt] A fim de garantir a segurança das instalações marítimas de produção de óleo e gás natural, parte do gás produzido é continuamente queimada, em função de condições específicas. Tais condições incluem paradas de emergência ou o alívio de inventário de gás devido a flutuações operacionais. A queima nestes ambientes acontece a uma grande faixa de vazões de gás, o que resulta em reduzido número de alternativas tecnológicas para sua medição. A medição de vazão a partir da tecnologia ultrasônica por tempo de trânsito vem sendo largamente utilizada, porém com incertezas relativamente elevadas, dadas as limitações da solução tecnológica. Devido a tais limitações, diversos órgãos reguladores da área de óleo e gás ao redor do mundo admitem diferentes percentuais para estimativa de incerteza da queima. No Brasil, a regulamentação estabelece um percentual máximo de 5 porcento para a queima de gás, não sendo porém específica quanto a que grandeza refere-se (vazão volumétrica ou volume). Esta dissertação traz um estudo sobre a incerteza de volumes horários, diários e mensais de gás produzidos por uma unidade de produção marítima por dezesseis meses, avaliando o impacto da incerteza na medição de vazão de queima sobre a incerteza dos volumes apurados. Foi avaliado o impacto de aspectos da medição ultrasônica de vazão de gás e da computação de volumes de produção a partir desta nos volumes apurados. Conclui-se que a medição de vazão e sua respectiva incerteza afetam de modo pouco significativo a incerteza dos volumes computados de queima. / [en] In order to assure safety at maritime oil & gas production facilities, part of the produced gas is continually burned (flared), depending upon specific operating conditions. These conditions include emergency shutdown and gas inventory relief due to process fluctuations. In such environments, gas flaring occurs at very large flow rate range, reducing the number of available technological choices for flow rate measurement. Transit-time ultrasonic flow measurement has been commonly used for this task, although with relatively high uncertainties due to technology limitations. Because of that, various oil & gas regulator authorities around the world impose different rules for flare measurement uncertainty. In Brazil, the regulation establishes a maximum percentage of 5 percent for flare measurement uncertainty, but it is not specific about the target (flow rate or volume). This dissertation presents a study on the effects of flow rate uncertainty on hourly, daily and monthly produced volume uncertainty in the maritime environment for a 16-month period, evaluating the impact of flare flow rate measurement on volume uncertainty. Aspects of gas transit-time ultrasonic flow rate measurement and volume computation over resulting volumes are evaluated. The conclusion is that flow rate measurement and its associated uncertainty have little effect on computed volume uncertainties.

Diplom thesis deals with the influence of typical pilot error during the landing maneuver in airplanes with maximum take-off mass 2250 kg. It contains basic information about the landing. The main attention is paid to the accident database, its subsequent evaluation and the proposal for a way to reduce these accidents. It also includes a survey of pilots.

Computer vision algorithms typically process real world image data acquired by cameras or video cameras. Such image data suffer from imperfections cause by the acquisition process. This paper focuses on simulation of the acquisition process on simulation of the acquisition process in order to enable rendering of images based on a 3D generated model. Imperfections, such as geometry distorion, chromatic aberration, depth of field effect, motion blur, vignetting and lens flare are considered.

The aim of this thesis was to implement a software that would be able to render, simulate and record a scene with walking pedestrians in real-time, with emphasis on rendering level of realism. The output of the application could serve as an input test data for people counting systems or similar systems for video recognition. The problem was divided into three major subproblems: character animation, artificial intelligence for character movement and advanced rendering techniques. The character animation problem is solved by the skeletal animation of the model. To achieve the characters moving in a scene autonomously path finding(A* algorithm) and group behaviors(steering behaviors) were implemented. Realism in a scene is added by implemented methods such as normal-mapping, variance shadow-mapping, deffered rendering, skydome, lens flare effect and screen space ambient occlusion. Optimaliaztion of the rendering was implemented using octree data structure for space partitioning. Rendering stage of a scene can be easily parametrized through implemented GUI. Implemented application provides the user with easy way of setting a scene with walking pedestrians, setting its visualization and to record the result.