Submitted by DANIEL MARTIN GASLAC GALLARDO (dmgg7900@hotmail.com) on 2016-12-13T16:40:12Z No. of bitstreams: 1 gaslac.pdf: 23986592 bytes, checksum: 41ffd339aeeb8444e4703d37a1753df4 (MD5) / Approved for entry into archive by Felipe Augusto Arakaki (arakaki@reitoria.unesp.br) on 2016-12-20T13:16:25Z (GMT) No. of bitstreams: 1 gallhardo_dmg_me_guara.pdf: 23986592 bytes, checksum: 41ffd339aeeb8444e4703d37a1753df4 (MD5) / Made available in DSpace on 2016-12-20T13:16:25Z (GMT). No. of bitstreams: 1 gallhardo_dmg_me_guara.pdf: 23986592 bytes, checksum: 41ffd339aeeb8444e4703d37a1753df4 (MD5) Previous issue date: 2016-10-11 / Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES) / Os novos dados obtidos do sistema de Plut˜ao, durante sua passagem pelo sistema em julho de 2015, est˜ao sendo enviados pela sonda New Horizons. Plut˜ao possui um conjunto de cinco sat´elites, Caronte (forma um sistema bin´ario com Plut˜ao), Estige, Nix, C´erberos e Hidra. A recente descoberta desses dois pequenos sat´elites, Estige e C´erberos, faz com que seja necess´ario reestudar essa regi˜ao externa, al´em da ´orbita de Caronte. Neste trabalho analisaremos a estabilidade da regi˜ao externa do sistema Plut˜ao-Caronte para um conjunto de part´ıculas-teste da ordem de cent´ımetros e micrometros sob a influˆencia gravitacional de todos os corpos do sistema de Plut˜ao e da press˜ao de radia¸c˜ao solar (para part´ıculas de micrometros). Essas part´ıculas estar˜ao inicialmente em ´orbitas excˆentricas e inclinadas; ser˜ao assumidos diferentes valores de excentricidade e inclina¸c˜ao. Resultados mostraram que para um conjunto de part´ıculas, originalmente localizadas no plano orbital do sistema de Plut˜ao, 10% colidiram com os corpos maiores e 25% foram ejetadas. J´a para o sistema de part´ıculas com ´orbitas inclinadas (I = 96.2 ◦ ), a maioria dessas part´ıculas s˜ao est´aveis. Apresentaremos os resultados obtidos para outros valores de inclina¸c˜ao e faremos a compara¸c˜ao com os resultados obtidos para um conjunto de part´ıculas microm´etricas da ordem de 1, 5 e 10µm. / The new data from the Pluto system during its passage through the system in July 2015, are being sent by the spacecraft NewHorizons. Pluto has a set of five satellites, Charon (forms a binary system with Pluto), Styx, Nix, Kerberos, Hydra. The recent discovery of these two small satellites, Styx and Kerberos, makes it necessary to restudy this outer region beyond the orbit of Charon. In this work we analyze the stability of the outer region Pluto-Charon system for a set of particle-test centimeters order and micron under gravitational influence of all bodies Pluto system and solar radiation pressure (for particle microns). These particles are initially eccentric and inclined orbits; They are assumed different eccentricity values and inclination. Results showed that for a set of particles originally located in orbital plane of Pluto system collided with 10% larger bodies and 25% were ejected. As for the particle system with inclined orbits (I = 96.2◦ ), most of these particles are stable. We present the results obtained for other of inclination values and make a comparison with the results obtained for a set of micrometric particles of the order of 1, 5 and 10µm.

Orientador: Rodolpho Vilhena de Moraes / Banca: Maria Cecilia França de Paula S. Zanardi / Banca: Sandro da Silva Fernandes / Resumo: Uma teoria para estudar o movimento orbital de satélites artificiais sobre efeitos do arrasto atmosférico e da pressão de radiação solar direta - considerando a sombra da Terrae alguns termos do geopotencial - é desenvolvida analiticamente. A sombra daTerra é modelada utilizando a função sombra, como introduzida por ferraz Mello: igual zero quando o satélite está na região de sombra e igual um quando é iluminado pelo sol. As componentes do arrasto são dadas por Vilhena de Moraes baseado no modelo atmosférico TD-88. O método de Hori para sistemas não canônicos é aplicado para resolver as equações de movimento. Um software para manipulação algébrica é fundamental apra fazer os cálculos necessários. Efeitos seculares e periódicos que influenciam no movimento orbital dos satélites artificiais são analisados. Expressões analíticas são apresentada explicitamente para os principais termos seculares nas variações dos elementos orbitais. É dada ênfase aos termos de acoplamento que surgem na solução do sistema de equações diferenciais. Utilizando dados orbitais do satélite CBERS-1 um estudo é feito para analisar ordens da variação do semi-eixo maior devidas as pertubações consideradas. / Abstract: A theory to study the orbital motion of artificial satellites under the effects of the atmospheric drag and of the direct solar radiatin pressure - considering the Earh's shadow and some terms of the geopotential - is developed analytically. The Earth shadow is modeled using the shadow function introduced by Ferrz Mello: equal zero when the satellite is in the shadow region and equal one when it is illuminated by the Sun. The drag components are given by Vilhena of Moraes based in the TD-88 temospheric model. The Hori's method for non-canonical systems is applied to solve the motion equation. A algebric manipulator software is fundamental to do the necessary calculations. Secular and periodic effects on the orbital motion of artificial satellites are analyzed. Analytic expressions are presented explicity for the main secular terms of the variations of the orbital elements. Emphasis is given to the coupling terms that appear in the solution of the differential euqatin systems. Using orbital data of the satellite CBERS-1 a study is done to analyze the order of magnitude of the variation of the semi-major axis due to the considered pertubation. / Mestre

Orientador: José Roberto de França Arruda / Dissertação (mestrado) - Universidade Estadual de Campinas, Faculdade de Engenharia Mecânica / Made available in DSpace on 2018-08-16T12:19:39Z (GMT). No. of bitstreams: 1 Coser_LucasFernando_M.pdf: 3895849 bytes, checksum: 203a0d7be9958aaa628e2b404ad566a9 (MD5) Previous issue date: 2010 / Resumo: Duas abordagens para a simulação do campo sonoro produzido por um arranjo esférico de alto-falantes são apresentadas e comparadas a resultados experimentais. Na primeira, modos estruturais obtidos da analise modal experimental da membrana são usados em simulações vibroacusticas por elementos de contorno no software LMS Virtual.Lab®. Na segunda, adota-se uma solução analítica baseada na expansão dos harmônicos esféricos de um padrão de velocidades sobre uma calota esférica. Os resultados são apresentados em termos de potencia sonora e de padrões de diretividade para o arranjo. No primeiro caso, são observadas as mesmas tendências na faixa de baixa freqüência em todas as curvas analisadas, havendo distorções consideráveis na faixa de alta freqüência para a solução analítica devido ao fato desta não incluir os efeitos dos modos estruturais da membrana. Por outro lado, os padrões de diretividade demonstram um alto grau de similaridade em todos os casos analisados e não são fortemente afetados pelos modos estruturais da membrana. As diferenças observadas nos resultados e as amplificações não realistas nas curvas de potencia sonora das simulações são causadas por três fatores principais: modos de cavidade acústica do arranjo esférico, desconsideração do acoplamento acústico entre os alto-falantes durante seus funcionamentos e utilização de um mesmo conjunto de FRFs para todos os alto-falantes. De uma forma geral, pode-se dizer que a simulação usando o modelo de membrana flexível melhora consideravelmente a previsão da potencia sonora na alta freqüência, o que não pode ser obtido com o modelo analítico comumente usado na analise de arranjos esféricos de alto-falantes / Abstract: Two approaches for sound field prediction of a spherical loudspeaker array operation are presented and compared to experimental measurements. In the first, real membrane modes from experimental modal analysis are used as input for BEM vibroacoustic simulations using LMS Virtual.Lab® software. In the second, an analytical solution based on the spherical harmonic expansion of an idealized velocity pattern over the spherical array is used. Results are presented in terms of sound power and directivity patterns, showing that the former has the same trend in all comparisons for the low frequency range, and that the analytical solution cannot be used for the high frequency range since it does not include the effect of the flexible membrane modes. Directivity patterns, however, show a good degree of similarity in all cases, and are not strongly affected by the flexible membrane modes. The differences found in the results and the unrealistic amplifications in the sound power curves from the simulations are caused mainly by three factors: acoustic cavity modes of the array, neglecting the acoustic coupling among loudspeakers for the operating condition and utilization of the same set of FRFs for all loudspeakers in the array. In a general way, it can be said that the flexible membrane modeling improves considerably the prediction of radiated sound power in the high frequency range, which cannot be obtained by the analytical model commonly used in the analysis of spherical loudspeaker arrays / Mestrado / Mecanica dos Sólidos e Projeto Mecanico / Mestre em Engenharia Mecânica

Solar radiation pressure (SRP) is one of the major non-gravitational forces acting on spacecraft. Acceleration by radiation pressure depends on the radiation flux; on spacecraft shape, attitude, and mass; and on the optical properties of the spacecraft surfaces. Precise modeling of SRP is needed for dynamic satellite orbit determination, space mission design and control, and processing of data from space-based science instruments. During Earth penumbra transitions, sunlight is passing through Earth's lower atmosphere and, in the process, its path, intensity, spectral composition, and shape are significantly affected. This dissertation presents a new method for highly physical SRP modeling in Earth's penumbra called Solar radiation pressure with Oblateness and Lower Atmospheric Absorption, Refraction, and Scattering (SOLAARS). The fundamental geometry and approach mirrors past work, where the solar radiation field is modeled using a number of light rays, rather than treating the Sun as a single point source. This dissertation aims to clarify this approach, simplify its implementation, and model previously overlooked factors. The complex geometries involved in modeling penumbra solar radiation fields are described in a more intuitive and complete way to simplify implementation. Atmospheric effects due to solar radiation passing through the troposphere and stratosphere are modeled, and the results are tabulated to significantly reduce computational cost. SOLAARS includes new, more efficient and accurate approaches to modeling atmospheric effects which allow us to consider the spatial and temporal variability in lower atmospheric conditions. A new approach to modeling the influence of Earth's polar flattening draws on past work to provide a relatively simple but accurate method for this important effect. Previous penumbra SRP models tend to lie at two extremes of complexity and computational cost, and so the significant improvement in accuracy provided by the complex models has often been lost in the interest of convenience and efficiency. This dissertation presents a simple model which provides an accurate alternative to the full, high precision SOLAARS model with reduced complexity and computational cost. This simpler method is based on curve fitting to results of the full SOLAARS model and is called SOLAARS Curve Fit (SOLAARS-CF). Both the high precision SOLAARS model and the simpler SOLAARS-CF model are applied to the Gravity Recovery and Climate Experiment (GRACE) satellites. Modeling results are compared to the sub-nm/s^2 precision GRACE accelerometer data and the results of a traditional penumbra SRP model. These comparisons illustrate the improved accuracy of the SOLAARS and SOLAARS-CF models. A sensitivity analyses for the GRACE orbit illustrates the significance of various input parameters and features of the SOLAARS model on results. The SOLAARS-CF model is applied to a study of penumbra SRP and the Earth flyby anomaly. Beyond the value of its results to the scientific community, this study provides an application example where the computational efficiency of the simplified SOLAARS-CF model is necessary. The Earth flyby anomaly is an open question in orbit determination which has gone unsolved for over 20 years. This study quantifies the influence of penumbra SRP modeling errors on the observed anomalies from the Galileo, Cassini, and Rosetta Earth flybys. The results of this study prove that penumbra SRP is not an explanation for or significant contributor to the Earth flyby anomaly. / Ph. D.

Sound pressure radiating from vibrating structures submerged in fluid, as in the case of a vibrating panel in a submarine hull, is usually undesirable. An optimal control methodology for the suppression of far-field acoustic radiation pressure from submerged structures has been developed by Meirovitch (ref. 1). The linear modal state feedback control law developed implies that the full state (displacements and velocities) is available, perhaps through measurements. However, in practice, it is not always feasible to measure the full modal state vector for feedback. To permit practical implementation of the feedback control law, an optimal stochastic state estimator, or Kalman-Bucy filter, has been developed here for incorporation into the control system design. The development has been specialized to a uniform simply supported rectangular plate. / Master of Science

Optical resonators such as silica micro-spheres and micro-toroids can support whispering gallery modes (WGMs), where light circulates near the resonator surface and is confined by the total internal reflection at the dielectric boundary. Such resonators can exhibit very high quality (Q) factors, since the resonator surface can maintain atomic level smoothness. The combination of high Q factors and small resonator volumes has led to a wide range of applications in sensing, optomechanics, nonlinear optics, and quantum optics. In this dissertation, we introduce a new type of whispering gallery resonators (WGRs) based on micro-droplets in an immiscible liquid-liquid system. Within such an all-liquid platform, it is possible to achieve highly nonlinear coupling between light and liquid that can potentially lead to single-photon level optical nonlinearity. Specifically, we experimentally characterize a droplet (D~500um) of index matching fluid submerged in the water as a high-Q optical resonator, where we use an optical fiber taper to couple light into the droplet through non-contact evanescent coupling. The highest Q-factor observed in the experiment is 2x10^7 which closely matches the upper limit of intrinsic Q-factor set by the material absorption. Given with such a high Q factor, the WGM can exert strong radiation pressure on the droplet interface, push it outward, increase the length of optical path, and produce a red-shift in WGM resonance. Our experimental results have found that the ratio of those resonance shifts and the optical power coupled into the resonator is approximately 60 fm/μW. The result closely matches to our steady-state estimation based on solving the coupled Maxwell-Navier-Stokes equation. To investigate the dynamic interplay of light and liquid, we develop a harmonic oscillator (HO) model to describe the time-domain behaviors of the coupled optofluidic system. We find a good agreement between theoretical predictions and our experimental data. The shift of WGM resonance can potentially be induced by thermal effects. To estimate the magnitude of thermal effects, we also investigate the thermally induced nonlinear behaviors of WGMs in a cylindrical fiber resonator (D~125um), where we change the mechanism of heat dissipation by changing the cladding material (e.g. air and water). For direct temperature measurements, we use a fiber optical resonator with a fiber Bragg grating (FBG) inscribed in the fiber core to observe temperature shifts induced by the high-Q WGMs. Our result shows that the temperature increase in the fiber resonator in the water is 0.13 C, whereas the fiber resonator in air shows ~4.5 C increase in temperature. Our results suggest that the relatively high thermal conductivity of water suppresses thermal nonlinearity by ~50 times, and that the red-shifts of WGMs can largely be attributed to radiation pressure effect. / Ph. D. / Optical resonators are used to confine incoming light and store its energy in a small volume. The quality of such resonators’ optical confinement is represented by quality factor (<i>Q</i>). Among different types of optical resonators, whispering gallery resonator (WGR) is well known for its high-<i>Q</i>, where strong optical confinement is achieved by the total internal reflection at the curved internal surface of spherical / cylindrical dielectric volume. The combination of high <i>Q</i> factors and small resonator volumes has led to a wide range of applications in sensing, optomechanics, nonlinear optics, and quantum optics. In this dissertation, we introduce a new type of WGR based on oil micro-droplet in water. Such an all-liquid platform enables highly nonlinear coupling between optical power and liquid matter that can potentially lead to optical nonlinearity at single-photon energy level. Specifically, we experimentally characterize an oil droplet (<i>D</i> ≈ 500 <i>um</i>) submerged in the water as a high-<i>Q</i> optical resonator, where we use a tapered optical fiber to inject optical power into the droplet. The highest <i>Q</i> of whispering gallery mode (WGM) observed in our experiment is 2×10⁷ and given with the high amplification of optical power in droplet, the WGM can exert strong radiation pressure on the droplet interface, push it outward, increase the length of optical path, and produce a red-shift in WGM resonance. Our experimental results have found that the ratio of those resonance shifts and the optical power coupled into the resonator is approximately 60 fm/<i>μ</i>W. The result closely matches to our steady-state estimation based on solving the coupled Maxwell-Navier-Stokes equation. To investigate the dynamic interplay of light and liquid, we develop a harmonic oscillator (HO) model to describe the time-domain behaviors of the coupled optofluidic system. We find a good agreement between theoretical predictions and our experimental data. The shift of WGM resonance can potentially be induced by thermal effects. To estimate the magnitude of thermal effects, we also investigate the thermally induced nonlinear behaviors of WGMs in a cylindrical fiber resonator (D ≈ 125 <i>um</i>), where we change the mechanism of heat dissipation by changing the media (e.g. air and water) surrounding the resonator. For direct temperature measurements, we use a fiber optical resonator with a temperature sensor equipped inside to observe temperature shifts induced by the high-<i>Q</i> WGMs. Our result shows that the temperature increase in the fiber resonator in the water is 0.13 °C, whereas the fiber resonator in air shows ~4.5 °C increase in temperature. Our results suggest that the relatively high thermal conductivity of water suppresses thermal nonlinearity by ~50 times, and that the red-shifts of WGMs can largely be attributed to radiation pressure effect.

<div>Aperiodic structures offer new functionalities for control, manipulation, and sensing that can benefit applications in all frequency ranges. We present a study of the influence of the degrees of freedom from a binary aperiodic nanostructure in free space, where each pixel is either the scatterer or the background, that uses a multivariate statistical analysis to examine the covariance matrix of the output field distributions. The total variance of the output fields and the rank can be evaluated to provide quantitative measurements of control. In addition, the field statistics provide an improved understanding of the scattering properties of aperiodic structures.</div><div><br></div><div><br></div><div><div>It has been proposed that structuring a metal surface can substantially increase the optical pressure over that possible with a planar interface. Based upon the forces on the mirrors of a one-dimensional asymmetric Fabry-Perot cavity, we show that the sum of the pressures on both mirrors increases through asymmetry and with quality factor. Using cavity quality factor as a measure, we present the physical basis of the enhanced pressure on a nanostructured metallic surface as being due to an array of asymmetric resonant cavities.</div></div><div><br></div><div><div>With use of optimized, aperiodic structures, more control and higher pressure should be possible. We present a design method by which the electromagnetic pressure on a nanostructured binary material can be controlled in terms of both the enhancement and the direction. This analysis offers new avenues for optomechanics.</div></div>

La pression de radiation acoustique est la force moyenne qu'une onde peut exercer sur un obstacle. Initialement, la faible manifestation de cette force ne suggérait pas d'applications potentielles. Néanmoins, avec l'avènement de sources acoustiques de haute puissance, il a rapidement été envisagé de manipuler de petits objets à distance par pression de radiation. Depuis, c'est via l'excitation d'ondes stationnaires dans des cavités que cette méthodologie connait son essor. Parallèlement, la pression de radiation de la lumière a rapidement permis de piéger et de manipuler des petits objets. Grâce à un laser fortement focalisé, la pince optique a donné une grande flexibilité aux techniques de manipulation sans contact et est devenue un outil fondamental pour de nombreuses disciplines scientifiques. Cependant, les faibles forces développées, les importantes intensités lumineuses requises et la petite taille des objets sont d'importantes limites tout particulièrement pour leur application en biologie.A l'heure actuelle, il n'existe pas l'équivalent de la pince optique en acoustique utilisant un unique faisceau. Le travail présenté donne un ensemble d'éléments théoriques et expérimentaux profitables pour la compréhension de la pression de radiation en acoustique et le dimensionnement d'une pince acoustique utilisant un unique faisceau ultrasonore : le vortex acoustique. Ce travail esquisse l'ébauche d'une nouvelle méthode de manipulation sans contact donnant une véritable dextérité de préhension. Les faibles intensités nécessaires associées aux larges forces développées sauront se montrer attractives pour imaginer un large panel de nouvelles applications scientifiques. / As an acoustic wave impinges an obstacle, a mean force is exerted on its surface. This so-called radiation pressure arises from the non linear interaction between the wave and the object.The early history of this force did not suggest any application of such a feeble effect. Nevertheless, as technological advances improved the prospects of new powerful sound sources, it was rapidly considered to use the acoustic radiation pressure as a mean of non-contact manipulation of small objects. Ever since, standing wave schemes excited in cavities has been the preferred strategy that is becoming considerably popular.In the same time, the radiation pressure of light was also recognised to trap and manipulate very small objects. Using a single focused laser beam, optical tweezers brought a great dexterity to non contact manipulation techniques and rapidly grew to become a fundamental tool in many scientific fields. However, the minuteness of the force, the high intensities required and the smallness of trappable objects are well-known limitations in particular for biological applications.Although optics and acoustics have shown many similarities, an acoustical analogue to optical tweezers using a single beam is yet to be demonstrated. Theoretical and experimental efforts are presented here and shed light on the underpinning mechanisms of single-beam acoustical tweezers. The analysis of a peculiar beam's radiation pressure, i.e. acoustical vortices, unveiled new characteristics for single-beam trapping. Our experimental demonstration along with the low intensities required and the large forces developed show promise for a wide spectrum of new scientific applications.

An increasing number of GPS applications require a high level of accuracy. To reduce the error contributed by the GPS ephemerides, an accurate modeling of the forces acting on GPS satellites is necessary. These forces can be categorized into gravitational and non-gravitational forces. The non-gravitational forces are a significant contribution to the total force on a GPS satellite but they are still not fully understood whereas the gravitational forces are well modeled. This study focuses on two non-gravitational forces: Solar Radiation Pressure (SRP) and the y-bias force. Different SRP models are available in the University of Texas Multi-Satellite Orbit Determination Program (MSODP). The recently developed University College London model was implemented for the purpose of this study. Several techniques to compute parameters associated with SRP models and the y-bias force during an orbit prediction were examined. Using the International GNSS Service (IGS) precise ephemerides as a reference, five different models were compared in the study. Satellite Laser Ranging (SLR) residuals were also studied to validate the approach. Results showed that the analytical UCL model performed as well as a purely empirical model such as the Extended CODE model. This is important since analytical models attempt to represent the physical phenomena and thus might be better suited to separate SRP from other forces. The y-bias force was then shown to have a once per revolution effect. The time evolution of the y-bias was found to be dependent on the SRP model used, the satellite Block type, the orbital plane, and the attitude of the satellite which suggests that estimates of y-bias contain errors from other sources, particularly the SRP models. The dependency of the y-bias evolution on the orbital plane suggests that the orientation of the plane towards the Sun is important. / text

The topic of this thesis is the theoretical analysis of theoptomechanical coupling effects in a high-finesse optical cavity, and the experimental realization of such a device.Radiation pressure exerted by light limits the sensitivity of high precision optical measurements. In particular, the sensitivity of interferometric measurements of gravitational wave is limited by the so called standard quantum limit. cavity with a movable mirror. The internal field stored in such cavity can be orders of magnitude greater than the input field, and it's radiation pressure force can change the physical length of the cavity. In turn, any change in the mirror's position changes the phase of the out put field. This optomechanical coupling leads to an intensity-dependent phase shift for thelight equivalent to an optical Kerr effect. Such a device can then be used for squeezing generation or quantum nondemolition measurements.In our experiment, we send a laser beam in to a high-finesse optical cavity with a movable mirror coated on a high Q-factor mechanical resonator. Quantum effects of radiation pressure become therefore, at low temperature, experimentally observable. However, we've shown that the phase of the reflected field is very sensitive to small mirror displacements, which indicate other possible applications of thistype of device like high precision displacements measurements. We've been able to observe the Brownian motion of the moving mirror. We've also used an auxiliary intensity modulated laser beam to optically excite the acoustic modes. We've finally obtained a sensitivity of2x10^(-19) m/sqrt(Hz), in agreement with theoretical prediction.