IP方法模拟硬盘读写头气膜润滑问题

本论文中采用IP方法模拟硬盘读写头的气膜润滑问题，并选择耗时但精准的DSMC方法作为该问题中IP方法的检验标准，IP方法计算得到的读写头表面压力分布及读写头所受净升力为读写头的设计提供可靠的参考数据。 首先，将读写头复杂表面简化为平面并假定尺寸为微米（远小于真实的毫米），微米尺寸时可以得到DSMC的模拟结果用于比较。IP法对该问题的模拟结果与DSMC的模拟结果完全吻合。 其次，选定一个真实的读写头表面几何，但仍然假定尺寸为微米。IP法在该问题的应用过程中遇到四点困难，我们提出或采取了相应的解决办法。在复杂表面几何的读写头气膜润滑问题中，IP法的模拟结果与DSMC的模拟结果也相符一致。 最后完成真实几何、真实尺寸（毫米）的读写头气膜润滑问题的模拟，这也是本论文的最终研究目标。IP法模拟该问题时需要采用大网格，为此我们构造二维检验模型验证了大网格的合理性。 真实几何读写头气膜润滑问题的模拟结果表明，在流场的局部区域压力沿着高度方向变化显著，这意味着读写头问题的传统计算方法（即概括性雷诺方程）在该局部区域不成立，故用它计算得到的结果值得认真检验，但文献中尚未给出过这类检验。这正是该论文的研究背景和采用新方法（IP方法）的原因。 本论文研究的问题属于过渡领域、低速流动问题，故本论文还介绍了该领域另外一种粒子模拟方法（LVDSMC方法）以及我们对该方法提出的一些改进。 关键词：硬盘读写头，气膜润滑，概括性雷诺方程，IP方法，DSMC方法，过渡领域，LVDSMC方法

Grain growth in protoplanetary disks

The majority of young, low-mass stars are surrounded by optically thick accretion disks. These circumstellar disks provide large reservoirs of gas and dust that will eventually be transformed into planetary systems. Theory and observations suggest that the earliest stage toward planet formation in a protoplanetary disk is the growth of particles, from sub-micron-sized grains to centimeter- sized pebbles. Theory indicates that small interstellar grains are well coupled into the gas and are incorporated to the disk during the proto-stellar collapse. These dust particles settle toward the disk mid-plane and simultaneously grow through collisional coagulation in a very short timescale. Observationally, grain growth can be inferred by measuring the spectral energy distribution at long wavelengths, which traces the continuum dust emission spectrum and hence the dust opacity. Several observational studies have indicated that the dust component in protoplanetary disks has evolved as compared to interstellar medium dust particles, suggesting at least 4 orders of magnitude in particle- size growth. However, the limited angular resolution and poor sensitivity of previous observations has not allowed for further exploration of this astrophysical process.

As part of my thesis, I embarked in an observational program to search for evidence of radial variations in the dust properties across a protoplanetary disk, which may be indicative of grain growth. By making use of high angular resolution observations obtained with CARMA, VLA, and SMA, I searched for radial variations in the dust opacity inside protoplanetary disks. These observations span more than an order of magnitude in wavelength (from sub-millimeter to centimeter wavelengths) and attain spatial resolutions down to 20 AU. I characterized the radial distribution of the circumstellar material and constrained radial variations of the dust opacity spectral index, which may originate from particle growth in these circumstellar disks. Furthermore, I compared these observational constraints with simple physical models of grain evolution that include collisional coagulation, fragmentation, and the interaction of these grains with the gaseous disk (the radial drift problem). For the parameters explored, these observational constraints are in agreement with a population of grains limited in size by radial drift. Finally, I also discuss future endeavors with forthcoming ALMA observations.

Demographic studies of extrasolar planets

Uncovering the demographics of extrasolar planets is crucial to understanding the processes of their formation and evolution. In this thesis, we present four studies that contribute to this end, three of which relate to NASA's Kepler mission, which has revolutionized the field of exoplanets in the last few years.

In the pre-Kepler study, we investigate a sample of exoplanet spin-orbit measurements---measurements of the inclination of a planet's orbit relative to the spin axis of its host star---to determine whether a dominant planet migration channel can be identified, and at what confidence. Applying methods of Bayesian model comparison to distinguish between the predictions of several different migration models, we find that the data strongly favor a two-mode migration scenario combining planet-planet scattering and disk migration over a single-mode Kozai migration scenario. While we test only the predictions of particular Kozai and scattering migration models in this work, these methods may be used to test the predictions of any other spin-orbit misaligning mechanism.

We then present two studies addressing astrophysical false positives in Kepler data. The Kepler mission has identified thousands of transiting planet candidates, and only relatively few have yet been dynamically confirmed as bona fide planets, with only a handful more even conceivably amenable to future dynamical confirmation. As a result, the ability to draw detailed conclusions about the diversity of exoplanet systems from Kepler detections relies critically on understanding the probability that any individual candidate might be a false positive. We show that a typical a priori false positive probability for a well-vetted Kepler candidate is only about 5-10%, enabling confidence in demographic studies that treat candidates as true planets. We also present a detailed procedure that can be used to securely and efficiently validate any individual transit candidate using detailed information of the signal's shape as well as follow-up observations, if available.

Finally, we calculate an empirical, non-parametric estimate of the shape of the radius distribution of small planets with periods less than 90 days orbiting cool (less than 4000K) dwarf stars in the Kepler catalog. This effort reveals several notable features of the distribution, in particular a maximum in the radius function around 1-1.25 Earth radii and a steep drop-off in the distribution larger than 2 Earth radii. Even more importantly, the methods presented in this work can be applied to a broader subsample of Kepler targets to understand how the radius function of planets changes across different types of host stars.

Developing and characterizing bulk metallic glasses for extreme applications

Metallic glasses have typically been treated as a “one size fits all” type of material. Every alloy is considered to have high strength, high hardness, large elastic limits, corrosion resistance, etc. However, similar to traditional crystalline materials, properties are strongly dependent upon the constituent elements, how it was processed, and the conditions under which it will be used. An important distinction which can be made is between metallic glasses and their composites. Charpy impact toughness measurements are performed to determine the effect processing and microstructure have on bulk metallic glass matrix composites (BMGMCs). Samples are suction cast, machined from commercial plates, and semi-solidly forged (SSF). The SSF specimens have been found to have the highest impact toughness due to the coarsening of the dendrites, which occurs during the semi-solid processing stages. Ductile to brittle transition (DTBT) temperatures are measured for a BMGMC. While at room temperature the BMGMC is highly toughened compared to a fully glassy alloy, it undergoes a DTBT by 250 K. At this point, its impact toughness mirrors that of the constituent glassy matrix. In the following chapter, BMGMCs are shown to have the capability of being capacitively welded to form single, monolithic structures. Shear measurements are performed across welded samples, and, at sufficient weld energies, are found to retain the strength of the parent alloy. Cross-sections are inspected via SEM and no visible crystallization of the matrix occurs.

Next, metallic glasses and BMGMCs are formed into sheets and eggbox structures are tested in hypervelocity impacts. Metallic glasses are ideal candidates for protection against micrometeorite orbital debris due to their high hardness and relatively low density. A flat single layer, flat BMG is compared to a BMGMC eggbox and the latter creates a more diffuse projectile cloud after penetration. A three tiered eggbox structure is also tested by firing a 3.17 mm aluminum sphere at 2.7 km/s at it. The projectile penetrates the first two layers, but is successfully contained by the third.

A large series of metallic glass alloys are created and their wear loss is measured in a pin on disk test. Wear is found to vary dramatically among different metallic glasses, with some considerably outperforming the current state-of-the-art crystalline material (most notably Cu₄₃Zr₄₃Al₇Be₇). Others, on the other hand, suffered extensive wear loss. Commercially available Vitreloy 1 lost nearly three times as much mass in wear as alloy prepared in a laboratory setting. No conclusive correlations can be found between any set of mechanical properties (hardness, density, elastic, bulk, or shear modulus, Poisson’s ratio, frictional force, and run in time) and wear loss. Heat treatments are performed on Vitreloy 1 and Cu₄₃Zr₄₃Al₇Be₇. Anneals near the glass transition temperature are found to increase hardness slightly, but decrease wear loss significantly. Crystallization of both alloys leads to dramatic increases in wear resistance. Finally, wear tests under vacuum are performed on the two alloys above. Vitreloy 1 experiences a dramatic decrease in wear loss, while Cu₄₃Zr₄₃Al₇Be₇ has a moderate increase. Meanwhile, gears are fabricated through three techniques: electrical discharge machining of 1 cm by 3 mm cylinders, semisolid forging, and copper mold suction casting. Initial testing finds the pin on disk test to be an accurate predictor of wear performance in gears.

The final chapter explores an exciting technique in the field of additive manufacturing. Laser engineered net shaping (LENS) is a method whereby small amounts of metallic powders are melted by a laser such that shapes and designs can be built layer by layer into a final part. The technique is extended to mixing different powders during melting, so that compositional gradients can be created across a manufactured part. Two compositional gradients are fabricated and characterized. Ti 6Al¬ 4V to pure vanadium was chosen for its combination of high strength and light weight on one end, and high melting point on the other. It was inspected by cross-sectional x-ray diffraction, and only the anticipated phases were present. 304L stainless steel to Invar 36 was created in both pillar and as a radial gradient. It combines strength and weldability along with a zero coefficient of thermal expansion material. Only the austenite phase is found to be present via x-ray diffraction. Coefficient of thermal expansion is measured for four compositions, and it is found to be tunable depending on composition.

Selective metallization on insulator surfaces with femtosecond laser pulses

We report selective metallization on surfaces of insulators ( glass slides and lithium niobate crystal) based on femtosecond laser modification combined with electroless plating. The process is mainly composed of four steps: (1) formation of silver nitrate thin films on the surfaces of glass or crystal substrates; (2) generation of silver particles in the irradiated area by femtosecond laser direct writing; (3) removal of unirradiated silver nitrate films; and (4) selective electroless plating in the modified area. We discuss the mechanism of selective metallization on the insulators. Moreover, we investigate the electrical and adhesive properties of the copper microstructures patterned on the insulator surfaces, showing great potential of integrating electrical functions into lab-on-a-chip devices. (C) 2007 Optical Society of America.

Estudo da expressão e participação de osteopontina durante a interação taquizoíto de Toxoplasma gondii célula hospedeira.

Toxoplasma gondii é um parasito do filo Apicomplexa que infecta uma grande variedade de hospedeiros, incluindo os humanos. O parasito invade a célula hospedeira por penetração ativa, com a participação das proteínas de suas organelas secretoras durante esse processo. Até o momento, somente um número limitado de proteínas secretoras tem sido descoberto, além disso, as moléculas efetoras envolvidas na invasão e sobrevivência do parasito não estão completamente compreendidas. A osteopontina (OPN) é uma glicofosfoproteína adesiva secretada, multifuncional, que contém o domínio arginina-glicina-ácido aspártico (RGD) de ligação à integrina, que está envolvida em uma variedade de eventos fisiológicos e patológicos, incluindo sinalização e sobrevivência celular. Pela primeira vez, nós demonstramos pelas técnicas de imunofluorescência e imunocitoquímica ultraestrutural que há uma intensa marcação para uma proteína OPN-like nos grânulos densos de taquizoítos de T. gondii extracelulares. O western blotting e o RT-PRC confirmaram a expressão de OPN-like nos taquizoítos. Nossos resultados também mostram que após a invasão dos macrófagos, a proteína OPN-like está localizada na membrana do vacúolo parasitóforo. Esses dados sugerem que os grânulos densos secretam uma proteína OPN-like, e nós podemos especular que essa proteína participa durante o processo de interação do parasito com as células hospedeiras. .

Relação dos sistemas de reparo de DNA em Escherichia coli K-12 com resistência a antibióticos, características adesivas e formação de biofilme

As espécies reativas de oxigênio (ERO) são geradas durante o metabolismo celular normal e podem produzir vários danos oxidativos no DNA, tais como lesões nas bases nitrogenadas ou sítios apurínico/apirimidínico (AP). Essas lesões podem acarretar acúmulo de sítios de mutações, caso esses danos não sejam reparados. Entretanto, as bactérias possuem vários mecanismos de defesa contra as ERO que desempenham um importante papel na manutenção da fisiologia. O objetivo deste trabalho foi o de avaliar se sistemas enzimáticos, como o reparo por excisão de bases (BER), sistema SOS e SoxRS, interferem em respostas como a sensibilidade aos antibióticos, aderência das células bacterianas a superfícies bióticas ou abióticas e formação de biofilme. Os mutantes utilizados no presente estudo são todos derivados de Escherichia coli K-12 e os resultados obtidos mostraram que, dos mutantes BER testados, o único que apresentou diferença no perfil de sensibilidade aos antimicrobiamos em relação à cepa selvagem (AB1157) foi o mutante xthA- (BW9091), deficiente em exonuclease III. No teste de aderência qualitativo realizado com linhagem de células HEp-2 (originária de carcinoma de laringe humana) foi observado que onze cepas da nossa coleção, apresentaram um padrão denominando like-AA, contrastando com o que era esperado para as cepas de E. coli utilizadas como controle negativo, que apresentam aderência discreta sem padrão típico. A aderência manose-sensível via fímbria do tipo I avaliada nesse estudo mostrou que essa fimbria, possui um papel relevante na intensidade da aderência e filamentação nessas cepas estudas. A filamentação é uma resposta SOS importante para que o genoma seja reparado antes de ser partilhado pelas células filhas. Além disso, com relação à formação de biofilme, oito cepas apresentaram um biofilme forte sendo que essa resposta não foi acompanhada pelo aumento da intensidade de filamentação. Nossos resultados em conjunto sugerem o envolvimento de estresse oxidativo na definição de parâmetros como sensibilidade a antimicrobianos, padrão e intensidade de aderência, filamentação e formação de biofilme nas amostras de E. coli K-12 avaliadas neste trabalho. Sugerimos que a aderência gera estresse oxidativo causando danos no DNA, o que leva a indução do sistema SOS resultando na resposta de filamentação observada.

Understanding planet formation through high precision photometry and spectroscopy

From studies of protoplanetary disks to extrasolar planets and planetary debris, we aim to understand the full evolution of a planetary system. Observational constraints from ground- and space-based instrumentation allows us to measure the properties of objects near and far and are central to developing this understanding. We present here three observational campaigns that, when combined with theoretical models, reveal characteristics of different stages and remnants of planet formation. The Kuiper Belt provides evidence of chemical and dynamical activity that reveals clues to its primordial environment and subsequent evolution. Large samples of this population can only be assembled at optical wavelengths, with thermal measurements at infrared and sub-mm wavelengths currently available for only the largest and closest bodies. We measure the size and shape of one particular object precisely here, in hopes of better understanding its unique dynamical history and layered composition.

Molecular organic chemistry is one of the most fundamental and widespread facets of the universe, and plays a key role in planet formation. A host of carbon-containing molecules vibrationally emit in the near-infrared when excited by warm gas, T~1000 K. The NIRSPEC instrument at the W.M. Keck Observatory is uniquely configured to study large ranges of this wavelength region at high spectral resolution. Using this facility we present studies of warm CO gas in protoplanetary disks, with a new code for precise excitation modeling. A parameterized suite of models demonstrates the abilities of the code and matches observational constraints such as line strength and shape. We use the models to probe various disk parameters as well, which are easily extensible to others with known disk emission spectra such as water, carbon dioxide, acetylene, and hydrogen cyanide.

Lastly, the existence of molecules in extrasolar planets can also be studied with NIRSPEC and reveals a great deal about the evolution of the protoplanetary gas. The species we observe in protoplanetary disks are also often present in exoplanet atmospheres, and are abundant in Earth's atmosphere as well. Thus, a sophisticated telluric removal code is necessary to analyze these high dynamic range, high-resolution spectra. We present observations of a hot Jupiter, revealing water in its atmosphere and demonstrating a new technique for exoplanet mass determination and atmospheric characterization. We will also be applying this atmospheric removal code to the aforementioned disk observations, to improve our data analysis and probe less abundant species. Guiding models using observations is the only way to develop an accurate understanding of the timescales and processes involved. The futures of the modeling and of the observations are bright, and the end goal of realizing a unified model of planet formation will require both theory and data, from a diverse collection of sources.

Hall coefficient and resistivity of an amorphous palladium-silicon alloy

The Hall coefficient and resistance in several specimens of an amorphous metallic alloy containing 80 at.% palladium and 20 at.% silicon have been investigated at temperatures between 4.2°K and room temperature. An ideal limiting behavior of these transport coefficients was analyzed on the basis of the nearly free electron model to yield a carrier density of 9 x 10²² cm.^-3, or about 1.7 electrons per palladium atom, and a mean free path of about 9Å which is almost constant with temperature. The deviations of the individual specimens from this ideal behavior, which were small but noticeable in the relative resistivity and much greater in the Hall coefficient, can be explained by invoking disk-shaped crystalline regions with low resistivity and a positive Hall coefficient. A detailed calculation shows how a volume fraction of such crystalline material too small to be noticed in X-ray diffraction could have a significant effect on the resistivity and a much greater effect on the Hall coefficient.

Avaliação dos métodos para análise da microinfiltração marginal em restaurações de resina composta classe V in vitro

O objetivo deste estudo foi comparar os resultados da microinfiltração marginal obtidos por diferentes meios de aquisição de imagens e métodos de mensuração da penetração de prata em restaurações de resina composta classe V, in vitro. Dezoito pré-molares humanos hígidos, recém extraídos, foram divididos em três grupos, de acordo com o tipo de instrumento para preparação cavitária utilizado. Grupo 1: ponta diamantada número 3100, em alta rotação. Grupo 2: broca carbide número 330, em alta rotação. Grupo 3: ponta CVDentus código 82137, em aparelho de ultrassom. Foram realizados preparos cavitários padronizados (3x4x2mm) classe V nas faces vestibular e lingual de todos os dentes, com margens oclusais em esmalte e cervicais em dentina/cemento. As cavidades foram restauradas com o sistema adesivo Solobond M (VOCO) e resina composta Grandio (VOCO), a qual foi inserida e fotoativada em três incrementos. Os corpos de prova ficaram imersos em água destilada por 24h a 37oC; receberam acabamento e polimento com discos SofLex (3M) e foram novamente armazenados em água destilada, por sete dias. Posteriormente, as superfícies dentárias foram coberta com duas camadas de esmalte para unhas vermelho, exceto as áreas adjacentes às restaurações. Os espécimes ficaram imersos em solução aquosa de nitrato de prata a 50% por 24h e em solução fotorreveladora por 2h e foram seccionados no sentido vestíbulo-lingual, passando pelo centro das restaurações, com disco diamantado em baixa rotação. As amostras foram polidas em politriz horizontal e analisadas por diferentes métodos. À extensão da microinfiltração foi atribuído escores de 0 a 3 através de análises por meio de estereomicroscópio tradicional e com leds e microscópio ótico. As imagens obtidas na lupa com leds e no microscópio ótico tiveram as áreas infiltradas medidas através do software AxioVision. O teste χ2 de McNemar-Bowker revelou concordância estatística entre estereomicroscópio tradicional e o com leds (p=0,809) durante análises semiquantitativas. Porém, houve diferenças significantes entre microscópio ótico e estereomicroscópios (p<0,001). Houve boa correlação entre análises semiquantitativas e quantitativas de acordo com o teste de Spearmann (p<0,001). O teste de Kruskall-Wallis não revelou diferenças estatisticamente significantes (p=0,174) entre os grupos experimentais na análise quantitativa por microscópio ótico, em esmalte. Ao contrário do que se observa com a mesma em lupa (p<0,001). Conclui-se que o método de atribuição de escores comumente aplicado com a lupa nos estudos da microinfiltração marginal é uma opção confiável para análise da microinfiltração.

New Insights from Aperiodic Variability of Young Stars

Nearly all young stars are variable, with the variability traditionally divided into two classes: periodic variables and aperiodic or "irregular" variables. Periodic variables have been studied extensively, typically using periodograms, while aperiodic variables have received much less attention due to a lack of standard statistical tools. However, aperiodic variability can serve as a powerful probe of young star accretion physics and inner circumstellar disk structure. For my dissertation, I analyzed data from a large-scale, long-term survey of the nearby North America Nebula complex, using Palomar Transient Factory photometric time series collected on a nightly or every few night cadence over several years. This survey is the most thorough exploration of variability in a sample of thousands of young stars over time baselines of days to years, revealing a rich array of lightcurve shapes, amplitudes, and timescales.

I have constrained the timescale distribution of all young variables, periodic and aperiodic, on timescales from less than a day to ~100 days. I have shown that the distribution of timescales for aperiodic variables peaks at a few days, with relatively few (~15%) sources dominated by variability on tens of days or longer. My constraints on aperiodic timescale distributions are based on two new tools, magnitude- vs. time-difference (Δm-Δt) plots and peak-finding plots, for describing aperiodic lightcurves; this thesis provides simulations of their performance and presents recommendations on how to apply them to aperiodic signals in other time series data sets. In addition, I have measured the error introduced into colors or SEDs from combining photometry of variable sources taken at different epochs. These are the first quantitative results to be presented on the distributions in amplitude and time scale for young aperiodic variables, particularly those varying on timescales of weeks to months.

Numerical modeling of optical levitation and trapping of the "stuck" particles with a pulsed optical tweezers

We present the theoretical analysis and the numerical modeling of optical levitation and trapping of the stuck particles with a pulsed optical tweezers. In our model, a pulsed laser was used to generate a large gradient force within a short duration that overcame the adhesive interaction between the stuck particles and the surface; and then a low power continuous - wave (cw) laser was used to capture the levitated particle. We describe the gradient force generated by the pulsed optical tweezers and model the binding interaction between the stuck beads and glass surface by the dominative van der Waals force with a randomly distributed binding strength. We numerically calculate the single pulse levitation efficiency for polystyrene beads as the function of the pulse energy, the axial displacement from the surface to the pulsed laser focus and the pulse duration. The result of our numerical modeling is qualitatively consistent with the experimental result. (C) 2005 Optical Society of America.

A Cerenkov-ΔΕ-Cerenkov detector for high energy cosmic ray isotopes and an accelerator study of ^(40)Ar & ^(56)Fe fragmentation

This thesis has two major parts. The first part of the thesis will describe a high energy cosmic ray detector -- the High Energy Isotope Spectrometer Telescope (HEIST). HEIST is a large area (0.25 m²sr) balloon-borne isotope spectrometer designed to make high-resolution measurements of isotopes in the element range from neon to nickel (10 ≤ Z ≤ 28) at energies of about 2 GeV/nucleon. The instrument consists of a stack of 12 NaI(Tl) scintilla tors, two Cerenkov counters, and two plastic scintillators. Each of the 2-cm thick NaI disks is viewed by six 1.5-inch photomultipliers whose combined outputs measure the energy deposition in that layer. In addition, the six outputs from each disk are compared to determine the position at which incident nuclei traverse each layer to an accuracy of ~2 mm. The Cerenkov counters, which measure particle velocity, are each viewed by twelve 5-inch photomultipliers using light integration boxes.

HEIST-2 determines the mass of individual nuclei by measuring both the change in the Lorentz factor (Δγ) that results from traversing the NaI stack, and the energy loss (ΔΕ) in the stack. Since the total energy of an isotope is given by Ε = γM, the mass M can be determined by M = ΔΕ/Δγ. The instrument is designed to achieve a typical mass resolution of 0.2 amu.

The second part of this thesis presents an experimental measurement of the isotopic composition of the fragments from the breakup of high energy ⁴⁰Ar and ⁵⁶Fe nuclei. Cosmic ray composition studies rely heavily on semi-empirical estimates of the cross-sections for the nuclear fragmentation reactions which alter the composition during propagation through the interstellar medium. Experimentally measured yields of isotopes from the fragmentation of ⁴⁰Ar and ⁵⁶Fe are compared with calculated yields based on semi-empirical cross-section formulae. There are two sets of measurements. The first set of measurements, made at the Lawrence Berkeley Laboratory Bevalac using a beam of 287 MeV/nucleon ⁴⁰Ar incident on a CH₂ target, achieves excellent mass resolution (σ_m ≤ 0.2 amu) for isotopes of Mg through K using a Si(Li) detector telescope. The second set of measurements, also made at the Lawrence Berkeley Laboratory Bevalac, using a beam of 583 MeV/nucleon ⁵⁶FeFe incident on a CH₂ target, resolved Cr, Mn, and Fe fragments with a typical mass resolution of ~ 0.25 amu, through the use of the Heavy Isotope Spectrometer Telescope (HIST) which was later carried into space on ISEE-3 in 1978. The general agreement between calculation and experiment is good, but some significant differences are reported here.

Influência do sistema de cimentação e do modo de ativação na resistência ao push-out de pinos de fibra de vidro

O objetivo deste estudo foi avaliar a influência do tipo de sistema de cimentação (condicionamento ácido total ou autoadesivo), do modo de ativação (autoativado ou dual), do terço do conduto radicular (cervical, médio ou apical) e da espessura do filme de cimento sobre a resistência de união de pinos de fibra de vidro cimentados em dentes humanos. Quarenta raízes foram incluídas em resina epóxi, submetidas a tratamento endodôntico e obturadas com guta percha e cimento endodôntico sem eugenol. Decorridos sete dias, os condutos foram preparados a uma profundidade de 10mm com brocas padronizadas do sistema dos pinos de fibra (WhitePost DC #2) e aleatoriamente divididos em 4 grupos, conforme o sistema de cimentação e o modo de ativação: (G1) RelyX ARC/Adper Scotchbond Multi-Purpose Plus (condicionamento ácido total), ativação dual, (G2) RelyX ARC/Adper Scotchbond Multi-Purpose Plus, autoativado, (G3) RelyX U100 (autoadesivo), dual e (G4) RelyX U100, autoativado. Após uma semana, cada raiz foi seccionada em máquina de corte, originando 6 fatias de 1 mm de espessura (n=60). Antes do ensaio de push-out cada fatia foi fotografada em ambas as faces, para determinação do raio dos pinos e da espessura do filme de cimento. Após o ensaio mecânico, novas imagens foram capturadas para determinação do modo de falha. Para automatizar a determinação da espessura de cimento, foi desenvolvida uma macro no software KS 400. Os dados foram estatisticamente analisados com ANOVA 3 fatores (resistência de união) e teste de Kruskall-Wallis (espessura do cimento). Comparações múltiplas foram realizadas com o teste Student-Newman-Keuls. Análise de regressão, modelo linear, foi empregada para verificar a correlação entre espessura do cimento e resistência de união. Todos os testes foram aplicados com α = 0,05. O fator cimento exerceu influência significativa para a resistência de união (p = 0,0402): o RelyX U100 apresentou a maior média. A ativação dual elevou os valores de resistência de união em comparação ao modo quimicamente ativado (p < 0,0001). Houve diferenças significantes entre os grupos, sendo G1 (22,4 4,0 MPa) > G3 (20,4 3,6 MPa) > G4 (17,8 5,2 MPa) > G2 (13,5 4,3 MPa). O terço do conduto não exerceu influência significativa sobre a resistência adesiva (p = 0,4749). As espessuras dos filmes de cimento foram estatisticamente diferentes nos diferentes terços: cervical (102 45 m) > médio (75 29 m) > apical (52 28m). Não foi observada forte correlação entre os valores de espessura e os de resistência ao push-out (r = - 0,2016, p = 0,0033). O tipo de falha predominante foi a mista, exceto para o G2, que apresentou 74% das falhas na interface cimento-pino. Dessa forma, o cimento autoadesivo apresentou melhor desempenho que o convencional, e ambos os sistemas duais, sobretudo o RelyX ARC, apresentaram dependência da fotoativação para atingirem maiores valores de resistência de união.

Efeito do selamento dentinário imediato na resistência de união de restaurações cerâmicas

O objetivo deste trabalho foi avaliar o efeito do selamento dentinário imediato na cimentação definitiva de restaurações cerâmicas (Empress2Ivoclar Vivadent), levando em consideração a influência de diferentes métodos de remoção dos restos de cimento provisório da superfície dentinária previamente selada. Para isso foram utilizados 72 molares, hígidos, conseguidos no banco de dentes da Universidade do Estado do Rio de Janeiro. Os dentes foram divididos em nove grupos, os três primeiros serviram como grupo controle, onde não houve contaminação com nenhum cimento provisório, sendo eles: G1, onde o selamento e a cimentação definitiva foram feitas 15 dias após a confecção dos preparos cavitários; G2, onde o selamento dentinário foi feito imediatamente após o preparo e a cimentação definitiva após 15 dias; G3, onde o preparo, selamento e cimentação definitiva foram feitos no mesmo momento. Os próximos grupos foram os do selamento tardio, onde o sistema adesivo foi aplicado somente no momento da cimentação. Nestes grupos, após o preparo foram cimentadas restaurações provisórias com um cimento livre de eugenol (Temp BondNE) e após 15 dias as restaurações provisórias foram removidas e os restos de cimento limpos com diferentes métodos: G4: remoção com instrumento manual; G5: remoção com jato de bicarbonato; G6: remoção com pontas de ultra-som; após esta limpeza o sistema adesivo foi aplicado e as restaurações cerâmicas cimentadas. Por último foram os grupos do selamento dentinário imediato, onde o sistema adesivo foi aplicado imediatamente após a confecção dos preparos cavitários e em seguida foi feita a cimentação das restaurações provisórias. Após 15 dias as restaurações provisórias foram removidas, os restos de cimento foram limpos com os diferentes métodos: G7: remoção com instrumento manual; G8: remoção com jato de bicarbonato; G9: remoção com pontas de ultra-som. Após a limpeza as restaurações cerâmicas foram cimentadas. Para todos os grupos o sistema adesivo utilizado foi o Optibond FL Kerr e o cimento resinoso foi o Rely X ARC3M/ESPE. Vinte e quatro horas após as cimentações cerâmicas os corpos de prova foram submetidos ao ensaio mecânico de push out em uma máquina de ensaios universais EMIC DL. Os valores de resistência de união foram obtidos em KgF, convertidos em MPa e analisados estatisticamente. O teste de ANOVA mostrou que houve diferença estatisticamente significante entre os grupos (p≤0,05) e em seguida o t-teste mostrou que a técnica do selamento imediato resultou nos melhores valores de resistência de união. Por último, o teste de comparações múltiplas Student-Newman-Keuls (Teste SNK) mostrou que o método de limpeza dos restos de cimento provisório da superfície dentinária apresenta influência na resistência de união das restaurações cerâmicas. Com base nos resultados pôde-se concluir que a técnica do selamento imediato promoveu maior resistência adesiva para as restaurações cerâmicas e quanto ao método de limpeza, o melhor resultado, independente da técnica adesiva utilizada, foi a remoção com as pontas de ultrasson.