Ultraviolet radiation (UVR) has been associated with various health outcomes, including skin cancers, vitamin D insufficiency, and multiple sclerosis. Measurement of UVR has been difficult, traditionally relying on subject recall. We investigated trends in satellite-derived UVB from 1978 to 2014 within the continental United States (US) to inform UVR exposure assessment and determine the potential magnitude of misclassification bias created by ignoring these trends. Monthly UVB data remotely sensed from various NASA satellites were used to investigate changes over time in the United States using linear regression with a harmonic function. Linear regression models for local geographic areas were used to make inferences across the entire study area using a global field significance test. Temporal trends were investigated across all years and separately for each satellite type due to documented differences in UVB estimation. UVB increased from 1978 to 2014 in 48% of local tests. The largest UVB increase was found in Western Nevada (0.145 kJ/m(2) per five-year increment), a total 30-year increase of 0.87 kJ/m(2). This largest change only represented 17% of total ambient exposure for an average January and 2% of an average July in Western Nevada. The observed trends represent cumulative UVB changes of less than a month, which are not relevant when attempting to estimate human exposure. The observation of small trends should be interpreted with caution due to measurement of satellite parameter inputs (ozone and climatological factors) that may impact derived satellite UVR nearly 20% compared to ground level sources. If the observed trends hold, satellite-derived UVB data may reasonably estimate ambient UVB exposures even for outcomes with long latency phases that predate the satellite record.

A method to calculate the Stokes parameters Q, U, as well as angle of polarization (AoP) from the new generation CIMEL Dual-Polar sun/sky radiometer CE318-DP polarized skylight measurements is developed in this thesis. Besides the degree of linear polarization (DoLP) and the total radiance I, the parameters Q, U, and AoP have much potential to improve retrievals of aerosol microphysical and chemical properties. However, they have not been derived based on the CE318-DP so far because they change with the reference plane that is hard to know due to an uncontrolled initial angle related to installation of the optical sensor head to the automated mount of this type of instrument. In this work, the polarization pattern of skylight with the direction of polarization perpendicular to the scattering plane (i.e., the principal plane in the solar principal plane geometry) is applied to correct the initial angle and then to obtained Q, U, and AoP. The perpendicular and parallel polarized radiances Ir and Il, as well as the linear depolarization ratio ρ are further derived after Q is known. A new polarized almucantar geometry based on CE318-DP is measured to illustrate abundant variation features of these parameters. These new polarization parameters in conjunction with DoLP and I are analyzed based on some typical long-term sites within the Sun/sky-radiometer Observation NETwork (SONET) and a joint site of the AErosol RObotic NETwork (AERONET) in China. Results calculated in this work are consistent with previous results, and generally comparable with the vector radiative transfer simulations and the measurements by other polarimetric instrument. Considering a 1°discrepancy of AoP, 3% fractional uncertainty in I and 0.005 uncertainty in DoLP propagated to Q and U, the uncertainties of Q in both of solar principal and almucantar planes and that of U in the almucantar geometry are acceptable.

O sol é a fonte de energia mais importante para todos os seres vivos no planeta Terra. Os sistemas concentrados de energia solar e fotovoltaica apresentaram avanços importantes na eficiência da conversão da irradiação solar em energia elétrica. A redução dos custos do equipamento necessário, combinada com um maior acesso ao conhecimento com a popularização da internet, permitiu que esta tecnologia se encontrasse em vários setores da sociedade. Neste estudo, analisou-se a eficiência energética de um painel solar com sistema de rastreamento de controle em circuito fechado baseado em fotoresistores. Este painel solar foi projetado e montado com tecnologia DIY em comparação com um painel de ângulo fixo. O sistema foi analisado em três condições atmosféricas diferentes: sol, parcialmente nublado e totalmente nublado. Os dados de corrente elétrica produzidos pelos dois sistemas e a carga consumida pelo painel do rastreador foram gravados automaticamente usando um sistema de coleta de dados para cada painel fotovoltaico. O sistema com rastreador mostrou uma produção de energia de 24,52% maior do que o painel fixo no período de maior radiação solar. Observou-se que a produção de energia do painel com sistema de rastreamento é maior durante períodos de ângulo de elevação inferior em relação ao horizonte. No entanto, a análise de eficiência energética do sistema de rastreamento apresentou uma comparação de geração de energia elétrica negativa em relação ao painel de ângulo fixo, e o painel com rastreador apresentou um custo elevado de 216,60% em relação ao painel em ângulo fixo. Portanto, não compensa o uso da tecnologia DIY nas condições testadas. / The sun is the most important source of energy for all living beings on planet Earth. Concentrated solar and photovoltaic systems have presented important advances in the efficiency of the conversion of solar irradiation to electric energy. The reduction in the costs of the necessary equipment, combined with greater access to knowledge with the popularization of the internet, has allowed this technology to be present in several sectors of society. In this study the energy efficiency of a solar panel with closed loop control tracker system based on photoresistors was analyzed. This solar panel was designed and assembled with DIY technology compared to a fixed-angle panel. The system was analyzed in three different atmospheric conditions: sunny, partly cloudy and totally cloudy. The electrical current data produced by the two systems and the load consumed by the tracker panel were automatically recorded using a data collection system for each photovoltaic panel. The system with tracker showed energy production of 24.52% higher than the fixed panel in the period of higher solar radiation. It was observed that the energy production of the panel with tracker system is higher during periods of lower elevation angle with respect to the horizon. However, the energy efficiency analysis of the tracking system presented a compared to of negative electric power generation in relation to the fixed-angle panel, and the panel with tracker presented a high cost of 216,60% in relation to the panel in fixed form. Therefore, it does not compensate for the use of DIY technology in the tested conditions.

Working with a three-dimensional shape that adjusts light seemed exciting. Venetian blinds became a basis and source of inspiration in my project. What is a Venetian blind? I arrived at the definition ”a surface of angleble pieces for sun adjustment”. From that simplified meaning I started making sketches of what an alternative model could look like. My sun shield consists of manual adjustable cylinders. The idea is that every adjustable piece, besides blocking sunlight, also can be a jig-saw-piece. Every cylinder has a simple décor on the blocking side. Depending on how the pieces are angled, different patterns are formed. The shadow effect will also be an adjustable pattern. My aim has been to make a prototype for alternative sun adjustment. Focus is on experiment with shape and user experience rather than technical perfection and efficiency. / <p>Program: Textildesignutbildningen</p><p>Uppsatsnivå: C</p>

Thesis (Ph. D.)--University of California, San Diego, 1982. / Vita. Includes bibliographical references (leaves 136-139).

Thesis--Guo li zheng zhi da xue. / Reproduced from ms. copy. Errata slip inserted. Includes bibliographical references (p. 833-859).

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Stellar model atmospheres are a fundamental tool for our understanding of stars. Because the chemical composition of stars cannot be measured directly, the inferred stellar parameters are model dependent. In recent years great progress has been made in the modeling of stellar atmospheres, allowing the relaxation of simplifying assumptions made in previous models. The use of new 3D model atmospheres to infer the solar chemical composition has resulted in a decrease of the solar metallicity. This result has caused some controversy and is being challenged. The main aim of this thesis is to ascertain if the new models of stellar atmospheres are realistic and can be trusted to derive the chemical composition of stars in general, and the Sun in particular. Other objectives also include the study of line formation in the Sun at high spatial resolution, and possible implications in the modeling. The Sun is the ideal test-bench for detailed analyses of stellar atmospheres. With the solar surface being resolved in great detail and at different viewing angles, a wealth of information can be gathered that allows for very robust tests of atmosphere models. The testing detailed here addresses several fronts. On one hand, the model�s temperature structure is directly tested with the classical tests of continuum centre-to-limb variations and absolute fluxes. On the other hand, the line formation is tested at different viewing angles and high spatial and spectral resolution. Here the main focus is on oxygen lines, as oxygen has an important contribution for the total solar metallicity. However, other lines are also tested. High quality data were specifically obtained for these line formation tests, using the Swedish 1-m Solar Telescope. For the temperature structure tests we find a surprisingly good agreement between the 3D model and the observations, surpassing even semi-empirical models. The solar 1D non-LTE models have a very similar behaviour to 1D LTE models, confirming that LTE is a good approximation in the solar photosphere. The 3D theoretical model performs consistently better than its 1D counterparts. The oxygen line formation tests are carried out in great detail, with a careful wavelength calibration, revised atomic data, and allowing for departures from LTE. Again we find a reassuring agreement between the 3D model predictions and the observations, both for the centre-to-limb variation of the lines and the line formation at high spatial resolution. The observations at different viewing angles also allowed the empirical determination of the role of hydrogen collisions with oxygen, important when deriving the oxygen abundance. The tests undertaken here show that the 3D model atmospheres are indeed very realistic. Their predicted temperature structure and velocity fields compare very favourably with observations of the Sun. Together with previous tests, this indicates they can be relied upon to derive the chemical composition of the Sun and similar late-type stars.

Thesis (M.M.) -- Florida State University, 2004. / Advisor: Matthew Shaftel, Florida State University, School of Music. Title and description from thesis home page (viewed 12-14-04). Document formatted into pages; contains 90 pages. Includes biographical sketch. Includes bibliographical references.