Optical designs for improved solar cell performance

The solar resource is the most abundant renewable resource on earth, yet it is currently exploited with relatively low efficiencies. To make solar energy more affordable, we can either reduce the cost of the cell or increase the efficiency with a similar cost cell. In this thesis, we consider several different optical approaches to achieve these goals. First, we consider a ray optical model for light trapping in silicon microwires. With this approach, much less material can be used, allowing for a cost savings. We next focus on reducing the escape of radiatively emitted and scattered light from the solar cell. With this angle restriction approach, light can only enter and escape the cell near normal incidence, allowing for thinner cells and higher efficiencies. In Auger-limited GaAs, we find that efficiencies greater than 38% may be achievable, a significant improvement over the current world record. To experimentally validate these results, we use a Bragg stack to restrict the angles of emitted light. Our measurements show an increase in voltage and a decrease in dark current, as less radiatively emitted light escapes. While the results in GaAs are interesting as a proof of concept, GaAs solar cells are not currently made on the production scale for terrestrial photovoltaic applications. We therefore explore the application of angle restriction to silicon solar cells. While our calculations show that Auger-limited cells give efficiency increases of up to 3% absolute, we also find that current amorphous silicion-crystalline silicon heterojunction with intrinsic thin layer (HIT) cells give significant efficiency gains with angle restriction of up to 1% absolute. Thus, angle restriction has the potential for unprecedented one sun efficiencies in GaAs, but also may be applicable to current silicon solar cell technology. Finally, we consider spectrum splitting, where optics direct light in different wavelength bands to solar cells with band gaps tuned to those wavelengths. This approach has the potential for very high efficiencies, and excellent annual power production. Using a light-trapping filtered concentrator approach, we design filter elements and find an optimal design. Thus, this thesis explores silicon microwires, angle restriction, and spectral splitting as different optical approaches for improving the cost and efficiency of solar cells.

Prevalência de HPV em adolescentes virgens e com atividade sexual

O Papilomavírus humano (HPV) é um vírus DNA bastante prevalente em estimativas mundiais, sendo a DST isolada mais frequente no mundo. Existem poucos dados sobre prevalência em adolescentes sem vida sexual ativa, havendo ainda muitos tabus nesta faixa etária. O presente estudo tem por objetivo identificar a prevalência de Papilomavírus humano através de biologia molecular em pacientes sem coitarca, comparando com um grupo de pacientes da mesma faixa etária com atividade sexual. Foram avaliadas 100 adolescentes com idade variando de 11 a 20 anos, com pelo menos dois anos pós-menarca, atendidas no período de janeiro de 2007 a janeiro de 2009 no ambulatório de ginecologia infantopuberal do Hospital Universitário Pedro Ernesto. Das 100 adolescentes, 50 apresentavam hímen íntegro e 50 relatavam atividade sexual regular. Para as pacientes sem coitarca (grupo 1) foi realizada uma coleta apenas de vestíbulo e para as pacientes com atividade sexual (grupo 2) foi realizada coleta de vagina e endocérvice. A pesquisa de DNA-HPV foi realizada por captura híbrida de 2 geração. Os resultados foram descritos em unidade relativa de luz. Para os dados categóricos foram aplicados os testes exato de Fisher. A positividade geral de DNA de HPV de alto e de baixo risco foi de 72%. No grupo 1 houve positividade do teste em 3 casos (6%). Já no grupo 2, 33 casos (66%) foram positivos para pelo menos um sítio. Material de vagina foi positivo em 30 casos (60%) e de colo em 27 casos (54%). Pode-se concluir que a positividade nas meninas com vida sexual ativa é alta. A infecção pelo HPV, ainda que pouco frequente, pode estar presente em meninas sem coitarca.

Dinâmica de crescimento de Cedrela odorata L. (Meliaceae) na Floresta Atlântica do Estado do Rio de Janeiro: fenologia, atividade cambial e dendrocronologia

Ao longo do século XX, poucos estudos de dendrocronologia foram desenvolvidos com espécies de ambientes tropicais, em função da crença de que as condições climáticas nessas regiões não apresentavam variações suficientemente marcantes e regulares para induzir um ritmo anual de crescimento radial. A realização de trabalhos sobre esse tema nas últimas décadas revelou que a formação de anéis de crescimento anuais nos trópicos pode estar associada a fatores diversos, como: existência de estação seca bem definida, ocorrência de inundações sazonais, respostas ao comportamento fenológico, respostas ao fotoperíodo e a ritmos endógenos. O presente estudo tem por objetivo compreender a dinâmica de crescimento radial de uma espécie da Mata Atlântica se desenvolvendo em ambiente natural. Para tanto, propôs-se: i) investigar a periodicidade da atividade cambial e dos fatores que a influenciam; ii) estimar a idade e taxa de crescimento diamétrico e iii) correlacionar os fatores ambientais com os anéis de crescimento, em indivíduos de Cedrela odorata L. Para o estudo da atividade cambial, foram obtidas amostras de caule a 1,30 m do solo, contendo periderme, faixa cambial e xilema e floema secundários, por métodos não destrutivos. A fenologia vegetativa e a frutificação dos indivíduos amostrados foram acompanhadas durante todo o período do experimento. O material coletado foi processado segundo técnicas usuais em Anatomia Vegetal e analisado sob microscopia óptica e de fluorescência. Os dados de fotoperíodo, precipitação, temperatura e fenologia vegetativa foram correlacionados à atividade cambial. Para o estudo dos anéis de crescimento, as coletas também foram realizadas a 1,30 m do solo, por meio de sonda de Pressler. As amostras obtidas foram polidas e analisadas sob microscópio estereoscópio, para demarcação e aferição do número de anéis de crescimento, e a largura dos anéis foi mensurada para a determinação das taxas de crescimento radial. A série histórica de temperatura e precipitação foi correlacionada à cronologia dos anéis de crescimento. Os resultados indicaram que a atividade cambial segue um ritmo anual de crescimento, correlacionado à sazonalidade do fotoperíodo, da precipitação e da fenologia vegetativa. A análise dos anéis de crescimento permitiu estimar a idade dos indivíduos e determinar a taxa média de incremento e as taxas de incremento diamétrico acumulado e incremento médio anual para a espécie no sítio de estudo. Os dados de incremento radial evidenciaram a ausência de relação entre a idade e o diâmetro das árvores. A análise da variação na largura dos anéis não apresentou correlações significativas com os fatores climáticos analisados.

Elemental composition of solar energetic particles

The Low Energy Telescopes on the Voyager spacecraft are used to measure the elemental composition (2 ≤ Z ≤ 28) and energy spectra (5 to 15 MeV /nucleon) of solar energetic particles (SEPs) in seven large flare events. Four flare events are selected which have SEP abundance ratios approximately independent of energy/nucleon. The abundances for these events are compared from flare to flare and are compared to solar abundances from other sources: spectroscopy of the photosphere and corona, and solar wind measurements.

The selected SEP composition results may be described by an average composition plus a systematic flare-to-flare deviation about the average. For each of the four events, the ratios of the SEP abundances to the four-flare average SEP abundances are approximately monotonic functions of nuclear charge Z in the range 6 ≤ Z ≤ 28. An exception to this Z-dependent trend occurs for He, whose abundance relative to Si is nearly the same in all four events.

The four-flare average SEP composition is significantly different from the solar composition determined by photospheric spectroscopy: The elements C, N and O are depleted in SEPs by a factor of about five relative to the elements Na, Mg, Al, Si, Ca, Cr, Fe and Ni. For some elemental abundance ratios (e.g. Mg/O), the difference between SEP and photospheric results is persistent from flare to flare and is apparently not due to a systematic difference in SEP energy/nucleon spectra between the elements, nor to propagation effects which would result in a time-dependent abundance ratio in individual flare events.

The four-flare average SEP composition is in agreement with solar wind abundance results and with a number of recent coronal abundance measurements. The evidence for a common depletion of oxygen in SEPs, the corona and the solar wind relative to the photosphere suggests that the SEPs originate in the corona and that both the SEPs and solar wind sample a coronal composition which is significantly and persistently different from that of the photosphere.

The streaming of 1.3-2.3 MeV cosmic-ray protons during periods between prompt solar particle events

The anisotropy of 1.3 - 2.3 MeV protons in interplanetary space has been measured using the Caltech Electron/Isotope Spectrometer aboard IMP-7 for 317 6-hour periods from 72/273 to 74/2. Periods dominated by prompt solar particle events are not included. The convective and diffusive anisotropies are determined from the observed anisotropy using concurrent solar wind speed measurements and observed energy spectra. The diffusive flow of particles is found to be typically toward the sun, indicating a positive radial gradient in the particle density. This anisotropy is inconsistent with previously proposed sources of low-energy proton increases seen at 1 AU which involve continual solar acceleration.

The typical properties of this new component of low-energy cosmic rays have been determine d for this period which is near solar minimum. The particles have a median intensity of 0.06 protons/ cm^(2)-sec-sr-MeV and a mean spectral index of -3.15.The amplitude of the diffusive anisotropy is approximately proportional to the solar wind speed. The rate at which particles are diffusing toward the sun is larger than the rate at which the solar wind is convecting the particles away from the sun. The 20 to 1 proton to alpha ratio typical of this new component has been reported by Mewaldt, et al. (1975b).

A propagation model with κ_(rr) assumed independent of radius and energy is used to show that the anisotropy could be due to increases similar to those found by McDonald, et al. (1975) at ~3 AU. The interplanetary Fermi-acceleration model proposed by Fisk (1976) to explain the increases seen near 3 AU is not consistent with the ~12 per cent diffusive anisotropy found.

The dependence of the diffusive anisotropy on various parameters is shown. A strong dependence of the direction of the diffusive anisotropy on the concurrently measured magnetic field direction is found, indicating a κ_⊥ less than κ_∥ to be typical for this large data set.

Nanophotonic Light Trapping In Thin Solar Cells

Over the last several decades there have been significant advances in the study and understanding of light behavior in nanoscale geometries. Entire fields such as those based on photonic crystals, plasmonics and metamaterials have been developed, accelerating the growth of knowledge related to nanoscale light manipulation. Coupled with recent interest in cheap, reliable renewable energy, a new field has blossomed, that of nanophotonic solar cells.

In this thesis, we examine important properties of thin-film solar cells from a nanophotonics perspective. We identify key differences between nanophotonic devices and traditional, thick solar cells. We propose a new way of understanding and describing limits to light trapping and show that certain nanophotonic solar cell designs can have light trapping limits above the so called ray-optic or ergodic limit. We propose that a necessary requisite to exceed the traditional light trapping limit is that the active region of the solar cell must possess a local density of optical states (LDOS) higher than that of the corresponding, bulk material. Additionally, we show that in addition to having an increased density of states, the absorber must have an appropriate incoupling mechanism to transfer light from free space into the optical modes of the device. We outline a portfolio of new solar cell designs that have potential to exceed the traditional light trapping limit and numerically validate our predictions for select cases.

We emphasize the importance of thinking about light trapping in terms of maximizing the optical modes of the device and efficiently coupling light into them from free space. To further explore these two concepts, we optimize patterns of superlattices of air holes in thin slabs of Si and show that by adding a roughened incoupling layer the total absorbed current can be increased synergistically. We suggest that the addition of a random scattering surface to a periodic patterning can increase incoupling by lifting the constraint of selective mode occupation associated with periodic systems.

Lastly, through experiment and simulation, we investigate a potential high efficiency solar cell architecture that can be improved with the nanophotonic light trapping concepts described in this thesis. Optically thin GaAs solar cells are prepared by the epitaxial liftoff process by removal from their growth substrate and addition of a metallic back reflector. A process of depositing large area nano patterns on the surface of the cells is developed using nano imprint lithography and implemented on the thin GaAs cells.

Observations of hydrogen and helium isotopes in solar cosmic rays

The isotopic composition of hydrogen and helium in solar cosmic rays provides a means of studying solar flare particle acceleration mechanisms since the enhanced relative abundance of rare isotopes, such as ²H, ³H and ³He, is due to their production by inelastic nuclear collisions in the solar atmosphere during the flare. In this work the Caltech Electron/Isotope Spectrometer on the IMP-7 spacecraft has been used to measure this isotopic composition. The response of the dE/dx-E particle telescope is discussed and alpha particle channeling in thin detectors is identified as an important background source affecting measurement of low values of (³He/⁴He).

The following flare-averaged results are obtained for the period, October, 1972 - November, 1973: (²H/¹H) = 7⁺¹⁰_-6 X 10^-6 (1.6 - 8.6 MeV/nuc), (³H/¹H) less than 3.4 x 10^-6 (1.2 - 6.8 MeV/nuc), (³He/⁴He) = (9 ± 4) x 10^-3, (³He/¹H) = (1.7 ± 0.7) x 10^-4 (3.1 - 15.0 MeV/nuc). The deuterium and tritium ratios are significantly lower than the same ratios at higher energies, suggesting that the deuterium and tritium spectra are harder than that of the protons. They are, however, consistent with the same thin target model relativistic path length of ~ 1 g/cm² (or equivalently ~ 0.3 g/cm² at 30 MeV/nuc) which is implied by the higher energy results. The ³He results, consistent with previous observations, would imply a path length at least 3 times as long, but the observations may be contaminated by small ³He rich solar events.

During 1973 three "³He rich events," containing much more ³He than ²H or ³H were observed on 14 February, 29 June and 5 September. Although the total production cross sections for ²H,³H and ³He are comparable, an upper limit to (²H/³He) and (³H/³He) was 0.053 (2.9-6.8 MeV/nuc), summing over the three events. This upper limit is marginally consistent with Ramaty and Kozlovsky's thick target model which accounts for such events by the nuclear reaction kinematics and directional properties of the flare acceleration process. The 5 September event was particularly significant in that much more ³He was observed than ⁴He and the fluxes of ³He and ¹H were about equal. The range of (³He/⁴He) for such events reported to date is 0.2 to ~ 6 while (³He/¹H) extends from 10^-3 to ~ 1. The role of backscattered and mirroring protons and alphas in accounting for such variations is discussed.

Solar photospheric and coronal abundances from solar energetic particle measurements

Observations of solar energetic particles (SEPs) from 22 solar flares in the 1977-1982 time period are reported. The observations were made by the Cosmic Ray Subsystem on board the Voyager 1 and 2 spacecraft. SEP abundances have been obtained for all elements with 3 ≤ Z ≤ 30 except Li, Be, B. F, Sc, V, Co and Cu. for which upper limits have been obtained. Statistically meaningful abundances of several rare elements (e.g., P, Cl, K, Ti, Mn) have been determined for the first time, and the average abundances of the more abundant elements have been determined with improved precision, typically a factor of three better than the best previous determinations.

Previously reported results concerning the dependence of the fractionation of SEPs relative to photosphere on first ionization potential (FIP) have been confirmed and amplified upon with the new data. The monotonic Z-dependence of the variation between flares noted by earlier studies was found to be interpretable as a fractionation, produced by acceleration of the particles from the corona and their propagation through interplanetary space, which is ordered by the ionic charge-to-mass ratio Q/ M of the species making up the SEPs. It was found that Q/M is the primary organizing parameter of acceleration and propagation effects in SEPs, as evidenced by the dependence on Q/M of time, spatial and energy dependence within flares and of the abundance variability from flare to flare.

An unfractionated coronal composition was derived by applying a simple Q/M fractionation correction to the observed average SEP composition, to simultaneously correct for all Q/M-correlated acceleration/propagation fractionation of SEPs. The resulting coronal composition agrees well with current XUV/X-ray spectroscopic measurements of coronal composition but is of much higher precision and is available for a much larger set of elements. Compared to spectroscopic photospheric abundances, the SEP-derived corona appears depleted in C and somewhat enriched in Cr (and possibly Ca and Ti).

An unfractionated photospheric composition was derived by applying a simple FIP fractionation correction to the derived coronal composition, to correct for the FIP-associated fractionation of the corona during its formation from photospheric material. The resulting composition agrees well with the photospheric abundance tabulation of Grevesse (1984) except for an at least 50% lower abundance of C and a significantly greater abundance of Cr and possibly Ti. The results support the Grevesse photospheric Fe abundance, about 50% higher than meteoritic and earlier solar values. The SEP-derived photospheric composition is not generally of higher precision than the available spectroscopic data, but it relies on fewer physical parameters and is available for some elements (C, N, Ne, Ar) which cannot be measured spectroscopically in the photosphere.

The isotopic composition of energetic particles emitted from a large solar flare

We report measurements of isotope abundance ratios for 5-50 MeV/nuc nuclei from a large solar flare that occurred on September 23, 1978. The measurements were made by the Heavy Isotope Spectrometer Telescope (HIST) on the ISEE-3 satellite orbiting the Sun near an Earth-Sun libration point approximately one million miles sunward of the Earth. We report finite values for the isotope abundance ratios ¹³C/¹²C, ¹⁵N/¹⁴N, ¹⁸O/¹⁶O, ²²Ne/ ²⁰Ne, ²⁵Mg/²⁴Mg, and ²⁶Mg/²⁴Mg, and upper limits for the isotope abundance ratios ³He/⁴He, ¹⁴C/¹²C, ¹⁷O/¹⁶O, and ²¹Ne/²⁰Ne.

We measured element abundances and spectra to compare the September 23, 1978 flare with other flares reported in the literature. The flare is a typical large flare with "low" Fe/O abundance (≤ 0.1).

For ¹³C/¹²C, ¹⁵N/¹⁴N, ¹⁸O/¹⁶O, ²⁵Mg/ ²⁴Mg, and ²⁶Mg/²⁴Mg, our measured isotope abundance ratios agree with the solar system abundance ratios of Cameron (1981). For neon we measure ²²Ne/²⁰Ne = 0.109 + 0.026 - 0.019, a value that is different with confidence 97.5% from the abundance measured in the solar wind by Geiss at al. (1972) of ²²Ne/²⁰Ne = 0.073 ± 0.001. Our measurement for ²²Ne/²⁰Ne agrees with the isotopic composition of the meteoritic component neon-A.

Separate arguments appear to rule out simple mass fractionation in the solar wind and in our solar energetic particle measurements as the cause of the discrepancy in the comparison of the apparent compositions of these two sources of solar material.

Magnetospheric access of solar particles and the configuration of the distant geomagnetic field

The access of 1.2-40 MeV protons and 0.4-1.0 MeV electrons from interplanetary space to the polar cap regions has been investigated with an experiment on board a low altitude, polar orbiting satellite (OG0-4).

A total of 333 quiet time observations of the electron polar cap boundary give a mapping of the boundary between open and closed geomagnetic field lines which is an order of magnitude more comprehensive than previously available.

Persistent features (north/south asymmetries) in the polar cap proton flux, which are established as normal during solar proton events, are shown to be associated with different flux levels on open geomagnetic field lines than on closed field lines. The pole in which these persistent features are observed is strongly correlated to the sector structure of the interplanetary magnetic field and uncorrelated to the north/south component of this field. The features were observed in the north (south) pole during a negative (positive) sector 91% of the time, while the solar field had a southward component only 54% of the time. In addition, changes in the north/south component have no observable effect on the persistent features.

Observations of events associated with co-rotating regions of enhanced proton flux in interplanetary space are used to establish the characteristics of the 1.2 - 40 MeV proton access windows: the access window for low polar latitudes is near the earth, that for one high polar latitude region is ~250 R_⊕ behind the earth, while that for the other high polar latitude region is ~1750 R_⊕ behind the earth. All of the access windows are of approximately the same extent (~120 R_⊕). The following phenomena contribute to persistent polar cap features: limited interplanetary regions of enhanced flux propagating past the earth, radial gradients in the interplanetary flux, and anisotropies in the interplanetary flux.

These results are compared to the particle access predictions of the distant geomagnetic tail configurations proposed by Michel and Dessler, Dungey, and Frank. The data are consistent with neither the model of Michel and Dessler nor that of Dungey. The model of Frank can yield a consistent access window configuration provided the following constraints are satisfied: the merging rate for open field lines at one polar neutral point must be ~5 times that at the other polar neutral point, related to the solar magnetic field configuration in a consistent fashion, the migration time for open field lines to move across the polar cap region must be the same in both poles, and the open field line merging rate at one of the polar neutral points must be at least as large as that required for almost all the open field lines to have merged in 0 (one hour). The possibility of satisfying these constraints is investigated in some detail.

The role played by interplanetary anisotropies in the observation of persistent polar cap features is discussed. Special emphasis is given to the problem of non-adiabatic particle entry through regions where the magnetic field is changing direction. The degree to which such particle entry can be assumed to be nearly adiabatic is related to the particle rigidity, the angle through which the field turns, and the rate at which the field changes direction; this relationship is established for the case of polar cap observations.

A quantitative investigation of the solar modulation of cosmic-ray protons and helium nuclei

The differential energy spectra of cosmic-ray protons and He nuclei have been measured at energies up to 315 MeV/nucleon using balloon- and satellite-borne instruments. These spectra are presented for solar quiet times for the years 1966 through 1970. The data analysis is verified by extensive accelerator calibrations of the detector systems and by calculations and measurements of the production of secondary protons in the atmosphere.

The spectra of protons and He nuclei in this energy range are dominated by the solar modulation of the local interstellar spectra. The transport equation governing this process includes as parameters the solar-wind velocity, V, and a diffusion coefficient, K(r,R), which is assumed to be a scalar function of heliocentric radius, r, and magnetic rigidity, R. The interstellar spectra, j_D, enter as boundary conditions on the solutions to the transport equation. Solutions to the transport equation have been calculated for a broad range of assumed values for K(r,R) and j_D and have been compared with the measured spectra.

It is found that the solutions may be characterized in terms of a dimensionless parameter, ψ(r,R) = ^∞∫_r V dr'/(K(r',R). The amount of modulation is roughly proportional to ψ. At high energies or far from the Sun, where the modulation is weak, the solution is determined primarily by the value of ψ (and the interstellar spectrum) and is not sensitive to the radial dependence of the diffusion coefficient. At low energies and for small r, where the effects of adiabatic deceleration are found to be large, the spectra are largely determined by the radial dependence of the diffusion coefficient and are not very sensitive to the magnitude of ψ or to the interstellar spectra. This lack of sensitivity to j_D implies that the shape of the spectra at Earth cannot be used to determine the interstellar intensities at low energies.

Values of ψ determined from electron data were used to calculate the spectra of protons and He nuclei near Earth. Interstellar spectra of the form j_D α (W - 0.25m)^-2.65 for both protons and He nuclei were found to yield the best fits to the measured spectra for these values of ψ, where W is the total energy and m is the rest energy. A simple model for the diffusion coefficient was used in which the radial and rigidity dependence are separable and K is independent of radius inside a modulation region which has a boundary at a distance D. Good agreement was found between the measured and calculated spectra for the years 1965 through 1968, using typical boundary distances of 2.7 and 6.1 A.U. The proton spectra observed in 1969 and 1970 were flatter than in previous years. This flattening could be explained in part by an increase in D, but also seemed to require that a noticeable fraction of the observed protons at energies as high at 50 to 100 MeV be attributed to quiet-time solar emission. The turnup in the spectra at low energies observed in all years was also attributed to solar emission. The diffusion coefficient used to fit the 1965 spectra is in reasonable agreement with that determined from the power spectra of the interplanetary magnetic field (Jokipii and Coleman, 1968). We find a factor of roughly 3 increase in ψ from 1965 to 1970, corresponding to the roughly order of magnitude decrease in the proton intensity at 250 MeV. The change in ψ might be attributed to a decrease in the diffusion coefficient, or, if the diffusion coefficient is essentially unchanged over that period (Mathews et al., 1971), might be attributed to an increase in the boundary distance, D.

Reprodutibilidade de um índice para diagnóstico e avaliação da atividade de lesões de cárie dentária na dentição decídua

O objetivo do presente estudo clínico é verificar a reprodutibilidade intra e interexaminadores de um critério de diagnóstico de cárie dentária (Nyvad et al. 1999) aplicado na dentição decídua, e avaliar o tempo médio necessário para a realização do exame clínico utilizando o referido critério. O mesmo é baseado na combinação de métodos visuais e táteis e propõe a diferenciação entre lesões ativas e inativas, tanto para lesões cavitadas quanto para não cavitadas. A amostra total consistiu de 80 crianças de três a sete anos de idade, de ambos os sexos, estudantes do Centro Educacional Terra Santa (Petrópolis/ RJ). Os responsáveis assinaram um termo de consentimento livre e esclarecido e o trabalho foi aprovado pelo Comitê de Ética em Pesquisa do HUPE-UERJ. Os exames foram realizados após escovação supervisionada, em consultório odontológico sob iluminação artificial, após 3-5s de secagem com ar comprimido, por dois examinadores treinados pelas autoras do índice e calibrados. As concordâncias intra e interexaminadores foram avaliadas pelo percentual de concordância (%) e pelo teste kappa (k), considerando a superfície dentária como unidade de análise e os seguintes pontos de corte: 1) hígida versus cariada; 2) ativa versus inativa; 3) descontinuidade versus hígida; e 4) cavitada versus hígida. O % e o valor de k para confiabilidade interexaminadores para cada ponto de corte foram: 1) % = 0,97 e k = 0,82 (IC: 0,80 - 0,85); 2) % = 0,98 e k = 0,80 (IC: 0,76 - 0,83); 3) % = 0,99 e k = 0,90 (IC: 0,88 - 0,93); 4) % = 99,0 e k = 0,95 (IC: 0,92 - 0,97). O % e o valor de k para confiabilidade intraexaminador para cada ponto de corte foram: 1) % = 0,98 e k = 0,86 (IC: 0,84 - 0,86); 2) % = 0,99 e k = 0,86 (IC: 0,83 - 0,89); 3) % = 0,99 e k = 0,94 (IC: 0,92 - 0,96); 4) % = 0,99 e k = 0,98 (IC: 0,96 - 0,99). O maior % de discordância (65,3% - 158/242) concentrou-se na diferenciação entre supefícies hígidas e lesões não cavitadas: 33,5% (81/242) entre superfície hígida e lesão não cavitada inativa; 26,0% (63/242), entre superfície hígida e lesão não cavitada ativa; e 5,8% (14/242), entre lesão não cavitada ativa e lesão não cavitada inativa. O tempo necessário para realização do exame clínico foi em média 226,5s (128,53). Conclui-se que o índice apresentou reprodutibilidade variando de substancial à quase perfeita e um tempo de exame viável, mostrando-se consistente e reproduzível para a realização de estudos clínicos de cárie dentária na dentição decídua.

Aproveitamento da água de chuva para fins não potáveis em uma atividade industrial: estudo de caso de uma edificação a ser construída, Rio de Janeiro, RJ

A escassez de água é um dos maiores desafios do nosso século. Parece mentira, uma vez que do planeta são ocupados por água. Essa abundância aparente leva-nos a considerar a água como um elemento barato, farto e inesgotável. Contudo, desse total, 97,5% são de água salgada, restando 2,5% de água doce, dos quais 1,75% formam geleiras, sendo, portanto, inacessíveis. E o pior: a exploração irracional da água doce armazenada nos lençóis subterrâneos, rios e lagos está ameaçando a magra fatia de 0,75% da água que pode ser usada pelo homem. Se a escassez e a poluição já são problemas concretos em muitos países, os quais já instituíram um efetivo gerenciamento de seus recursos hídricos, no Brasil a preocupação de cientistas e ambientalistas nem sempre é levada a sério. Afinal, temos mais de 12% da água potável do globo. No entanto, esta riqueza é extremamente mal distribuída: cerca de 80% estão na região amazônica; os 20% restantes distribuem-se desigualmente pelo país, atendendo a 95% da população. Cada vez que chove, milhões de litros de água, que normalmente deveram se infiltrar no solo correm pelos telhados e pelo asfalto até acabar em um rio poluído, sem nenhuma possibilidade de uso. E essa água pode e deve ser aproveitada, tanto para evitar enchentes quanto para economizar recursos hídricos e financeiros. Dessa forma, o objetivo deste trabalho foi o de estruturar um projeto de um sistema de coleta e aproveitamento da água de chuva, para fins não potáveis, para uma edificação a ser construída nas instalações de uma indústria de reparo e construção naval. Para tanto, foi apresentada uma metodologia cuja tecnologia para captação e aproveitamento da água de chuva baseou-se num levantamento bibliográfico e foi validada através da aplicação em um estudo de caso. Espera-se que este trabalho seja o ponto de partida para muitos outros dentro da indústria, procurando incentivar o aproveitamento da água de chuva para consumo não potável e criando assim uma consciência ecológica em todos os níveis da empresa, contribuindo dessa forma para a sustentabilidade.

Solar System Small-Body Demographics with the Palomar Transient Factory Survey

Observational studies of our solar system's small-body populations (asteroids and comets) offer insight into the history of our planetary system, as these minor planets represent the left-over building blocks from its formation. The Palomar Transient Factory (PTF) survey began in 2009 as the latest wide-field sky-survey program to be conducted on the 1.2-meter Samuel Oschin telescope at Palomar Observatory. Though its main science program has been the discovery of high-energy extragalactic sources (such as supernovae), during its first five years PTF has collected nearly five million observations of over half a million unique solar system small bodies. This thesis begins to analyze this vast data set to address key population-level science topics, including: the detection rates of rare main-belt comets and small near-Earth asteroids, the spin and shape properties of asteroids as inferred from their lightcurves, the applicability of this visible light data to the interpretation of ultraviolet asteroid observations, and a comparison of the physical properties of main-belt and Jovian Trojan asteroids. Future sky-surveys would benefit from application of the analytical techniques presented herein, which include novel modeling methods and unique applications of machine-learning classification. The PTF asteroid small-body data produced in the course of this thesis work should remain a fertile source of solar system science and discovery for years to come.

Plasma loop and strapping field dynamics: reproducing solar eruptions in the laboratory

Coronal mass ejections (CMEs) are dramatic eruptions of large, plasma structures from the Sun. These eruptions are important because they can harm astronauts, damage electrical infrastructure, and cause auroras. A mysterious feature of these eruptions is that plasma-filled solar flux tubes first evolve slowly, but then suddenly erupt. One model, torus instability, predicts an explosive-like transition from slow expansion to fast acceleration, if the spatial decay of the ambient magnetic field exceeds a threshold.

We create arched, plasma filled, magnetic flux ropes similar to CMEs. Small, independently-powered auxiliary coils placed inside the vacuum chamber produce magnetic fields above the decay threshold that are strong enough to act on the plasma. When the strapping field is not too strong and not too weak, expansion force build up while the flux rope is in the strapping field region. When the flux rope moves to a critical height, the plasma accelerates quickly, corresponding to the observed slow-rise to fast-acceleration of most solar eruptions. This behavior is in agreement with the predictions of torus instability.

Historically, eruptions have been separated into gradual CMEs and impulsive CMEs, depending on the acceleration profile. Recent numerical studies question this separation. One study varies the strapping field profile to produce gradual eruptions and impulsive eruptions, while another study varies the temporal profile of the voltage applied to the flux tube footpoints to produce the two eruption types. Our experiment reproduced these different eruptions by changing the strapping field magnitude, and the temporal profile of the current trace. This suggests that the same physics underlies both types of CME and that the separation between impulsive and gradual classes of eruption is artificial.