Orientador: Lourenço Correr Sobrinho / Tese (doutorado) - Universidade Estadual de Campinas, Faculdade de Odontologia de Piracicaba / Made available in DSpace on 2018-08-13T08:17:31Z (GMT). No. of bitstreams: 1 Biscaro_SandroLuis_D.pdf: 1231684 bytes, checksum: 94a704d3aec635c1016ca3eb4b5ced3a (MD5) Previous issue date: 2009 / Resumo: O objetivo neste estudo foi avaliar a influência de diferentes doses de radiação X na resistência de união de restaurações adesivas à dentina, mediadas por sistemas que apresentam diferentes estratégias para união. Foram obtidas superfícies planas de dentina em molares humanos e amostras cilíndricas foram construídas com compósito (Z250, 3M ESPE), para o teste de resistência de união ao microcisalhamento, utilizando três sistemas de união: um adesivo de condicionamento total de dois passos (Single Bond 2 - SB2, 3M ESPE), um autocondicionante de dois passos (Clearfil SE Bond - CSE, Kuraray) e um autocondicionante de passo único (Adper Prompt - ADP, 3M ESPE). As amostras foram separadas em 4 grupos (n= 10), de acordo com a dose de radiação X: 0 (controle), 5, 35 ou 70 Gy. A radiação foi direcionada para a superfície dos cilindros de compósito. O teste de microcisalhamento foi realizado após 24 h, e os modos das falhas classificadas com aumento de 200x. Os dados foram submetidos à Análise de Variância dois fatores e teste de Holm-Sidak's (p < 0,05). Uma análise de regressão não-linear foi conduzida com "resistência de união" como variável dependente. Os resultados de resistência de união (MPa) foram dose e material dependentes. SB2: controle > 5 = 35 > 70; CSE: controle = 5 > 35 = 70; ADP: controle = 5 = 35 = 70. Generalizando, SB2 > CSE > ADP. A análise de regressão não-linear mostrou que, em geral, um aumento na dose de radiação promoveu diminuição na resistência de união (R2 < 0,905). Os modos de falhas foram dependentes do sistema de união, mas, em geral, não houve influência significativa da radiação. Concluindo, a radiação-X apresentou um efeito dosedependente significativamente negativo na adesão à dentina. / Abstract: This study investigated the influence of different x-ray radiation doses on the bond strength of adhesive restorations to dentin mediated by systems presenting distinct bonding strategies. Flat dentin surfaces in human molars were obtained and cylinder-shaped specimens for the microshear bond test were build-up with a composite (Z250, 3M ESPE), using three adhesive systems: a total-etch, two-step (Single Bond 2 - SB2, 3M ESPE), a self-etching, two-step (Clearfil SE Bond - CSE, Kuraray), or a self-etching, single step (Adper Prompt - ADP, 3M ESPE). The specimens were assigned to 4 groups (n = 10), according to the x-ray dose: 0 (control), 5, 35 or 70 Gy. Radiation was directed to the surface of the resin cylinders. Microshear testing was conducted after 24 h, and the failure modes classified under magnification (200x). Data were submitted to two-way ANOVA and Holm-Sidak's test (p<0.05). A non-linear regression analysis was carried out with 'bond strength' as dependent variable. Bond strength results were dose- and material-dependent. SB2: control > 5 = 35 > 70; CSE: control = 5 > 35 = 70; ADP: control = 5 = 35 = 70. Generally, SB2 > CSE > ADP. The non-linear regression plots showed that in general, an increase in radiation dose may predict a decrease in bond strength (R2 = 0.905). Failure modes were dependent on the bonding system, generally with no significant influence of radiation. X-ray radiation presented a significant, dose-dependent detrimental effect on the bond to dentin. / Doutorado / Radiologia Odontologica / Doutor em Radiologia Odontológica

The ultimate aim of this work is to develop a laboratory model of large area, xenon-filled, proportional counter, that has good spatial resolution in conjunction with optimum spectral resolution in the energy range 1 to 10 keV. The results of initial development on a 10cm x 10cm imaging counter are first described. The most important effect established in this work is the dependence of spatial resolution on the quench gas. This effect is also observed to be a function of detector size. The mechanism proposed is that secondary electrons liberated by UV photons from the avalanche cause fluctuations in the centroid position of the induced charge distribution. Space charge effects are also observed at the gains required for imaging, which implies that the detector is semi-proportional. This causes degraded energy resolution at the high gains that are used for imaging. The linearity of a xenon imaging counter is found to be poor in the axis perpendicular to the anode wire direction. The use of a long drift region and different quench gases are investigated together with their effect on linearity and spatial resolution in the axis perpendicular to the anode wire direction. Finally, the construction and evaluation of a large area counter 30cm square is described. It is shown that this device produces excellent results (spatial resolution of 1.2mm FWHM and an energy resolution of 27% at 6 keV). Methods of improving the performance of the instrument are also discussed.

No description available.

No description available.

No description available.

The cosmic X-ray background was discovered at the dawn of the X-ray astronomy: during the first successful rocket flight launched to study the X-ray emission from the Moon, the presence of a residual diffuse emission was also "serendipitously" revealed. In the intervening decades, observations with improving angular and spectral resolution have enhanced our understanding of the components that make up this background. Above 1 keV, the emission is highly isotropic on large angular scales, has extragalactic origin, and about ~80 percent has been resolved into discrete sources (Mushotzky et al. 2000, Hasinger et al. 1998). Our current interpretation of the diffuse X-ray emission below 1 keV uses a combination of 5 components, solar wind charge exchange, Local Bubble, Galactic halo, intergalactic gas, and unresolved point sources. Resolving the different components is made particularly difficult by the similar spectral emission of most components, X-ray lines of heavily ionized metals, which are poorly resolved by the energy resolution of CCD cameras onboard current X-ray satellites with typical observing times. The goal of this investigation is to assess the integral emission of the major components of the diffuse Soft X-Ray Background. In the first part of my project, I analyzed the shadow observations performed with XMM-Newton and Suzaku X-ray observatories. Shadow observations offer a tool to separate the fore ground component, due to the Local Bubble and, possibly, charge exchange within the solar system, from the background component, due primarily to the Galactic Halo and unidentified point sources. In the second part of my project, I studied the contribution of unresolved point sources and intergalactic medium to the diffuse Soft X-ray Background.

published_or_final_version / Physics / Master / Master of Philosophy

An increasing number of fields would benefit from a single analytical probe that can characterise bulk objects that vary in morphology and/or material composition. These fields include security screening, medicine and material science. In this study the X-ray region is shown to be an effective probe for the characterisation of materials. The most prominent analytical techniques that utilise X-radiation are reviewed. The study then focuses on methods of amalgamating the three dimensional power of kinetic depth X-ray (KDFX) imaging with the materials discrimination of angular dispersive X-ray diffraction (ADXRD), thus providing KDEX with a much needed material specific counterpart. A knowledge of the sample position is essential for the correct interpretation of diffraction signatures. Two different sensor geometries (i.e. circumferential and linear) that are able to collect end interpret multiple unknown material diffraction patterns and attribute them to their respective loci within an inspection volume are investigated. The circumferential and linear detector geometries are hypothesised, simulated and then tested in an experimental setting with the later demonstrating a greater ability at discerning between mixed diffraction patterns produced by differing materials. Factors known to confound the linear diffraction method such as sample thickness and radiation energy have been explored and quantified with a possible means of mitigation being identified (i.e. via increasing the sample to detector distance). A series of diffraction patterns (following the linear diffraction appoach) were obtained from a single phantom object that was simultaneously interrogated via KDEX imaging. Areas containing diffraction signatures matched from a threat library have been highlighted in the KDEX imagery via colour encoding and match index is inferred by intensity. This union is the first example of its kind and is called diffraction enhanced KDEX imagery. Finally an additional source of information obtained from object disparity is explored as an alternative means of calculating sample loci. This offers a greater level of integration between these two complimentary techniques as object disparity could be used to reinforce the results produced by the linear diffraction geometry.

Thesis (Ph. D.)--Michigan State University. Dept. of Astronomy and Astrophysics, 2008. / Title from PDF t.p. (viewed on July 23, 2009) Includes bibliographical references (p. 238-251). Also issued in print.

Lynx is a concept under study for prioritization in the 2020 Astrophysics Decadal Survey. Providing orders of magnitude increase in sensitivity over Chandra, Lynx will examine the first black holes and their galaxies, map the large-scale structure and galactic halos, and shed new light on the environments of young stars and their planetary systems. In order to meet the Lynx science goals, the telescope consists of a high-angular resolution optical assembly complemented by an instrument suite that may include a High Definition X-ray Imager, X-ray Microcalorimeter and an X-ray Grating Spectrometer. The telescope is integrated onto the spacecraft to form a comprehensive observatory concept. Progress on the formulation of the Lynx telescope and observatory configuration is reported in this paper.