Dor de origem periodontal e de mucosa: eventos agudos na atenção básica

Este objeto começa destacando que situações de dor de origem periodontal são eventos muito co¬muns no cotidiano do cirurgião dentista, pois estão relacionadas principalmente à presença das do¬enças periodontais. Ressalta a importância do estudo das gengivites e periodontites como doenças isoladas ou como fatores contribuintes para o estabelecimento de doenças periodontais mais graves. Lembra que é obrigação do cirurgião-dentista diagnosticar e promover a conduta necessária para prevenção e tratamento ou para encaminhamento. Aborda lesões da mucosa bucal que causam sintomatologia dolorosa. Relata que dores de origem periodontal têm, em sua grande maioria, etiologia relacionada ao acúmulo de placa dentária e, portanto, sua prevenção está relacionada diretamente com a qualidade da higiene bucal. Explica o conceito e a classificação da dor de origem periodontal e na mucosa, detalhando agravos e doenças que causam dor de origem periodontal (impacção alimentar; gengivite relacionada à placa dentária; periodontite crônica relacionada à placa dentária; abscesso periodontal; pericoronarite; gengivite ulcerativa necrosante – GUN; gengivites descamativas) e agravos e doenças que causam dor na mucosa (mucosite; estomatite aftosa recorrente; gengivoestomatite herpética aguda – GEHA; doenças imunomediadas). Detalha as formas de avaliação e diagnóstico diferencial dos casos, compreendendo o modo como tais situações se apresentam em eventos agudos. Explica a realização dos procedimentos de avaliação, tornando o diagnóstico mais preciso e a assistência mais resolutiva, e detalha a abordagem inicial dos casos. Ressalta a extrema importância do acompanhamento pelos profissionais da Atenção Básica dos casos encaminhados aos outros níveis de atenção, na perspectiva da continuidade do cuidado. Finaliza indicando, em anexo, a prescrição de medicamentos em situações de dor de origem periodontal e na mucosa e a importância do conhecimento farmacológico do cirurgião-dentista, que não pode se restringir apenas a prescrição de analgésicos, antibióticos e anti-inflamatórios.1.0Ministério da Saúde/OPAS/OM

High Dimensional Classification with combined Adaptive Sparse PLS and Logistic Regression

Motivation: The high dimensionality of genomic data calls for the development of specific classification methodologies, especially to prevent over-optimistic predictions. This challenge can be tackled by compression and variable selection, which combined constitute a powerful framework for classification, as well as data visualization and interpretation. However, current proposed combinations lead to instable and non convergent methods due to inappropriate computational frameworks. We hereby propose a stable and convergent approach for classification in high dimensional based on sparse Partial Least Squares (sparse PLS). Results: We start by proposing a new solution for the sparse PLS problem that is based on proximal operators for the case of univariate responses. Then we develop an adaptive version of the sparse PLS for classification, which combines iterative optimization of logistic regression and sparse PLS to ensure convergence and stability. Our results are confirmed on synthetic and experimental data. In particular we show how crucial convergence and stability can be when cross-validation is involved for calibration purposes. Using gene expression data we explore the prediction of breast cancer relapse. We also propose a multicategorial version of our method on the prediction of cell-types based on single-cell expression data. Availability: Our approach is implemented in the plsgenomics R-package.Comment: 9 pages, 3 figures, 4 tables + Supplementary Materials 8 pages, 3 figures, 10 table

Hybrid multi-grids simulations of Ganymede's magnetosphere

International audienceThe Jovian satellite Ganymede is the biggest moon of our solar system. One of the main motivation of our interest for this moon is its own intrinsic magnetic field, which has been discovered during the Galileo mission (Kivelson et al. 1996). The magnetic field of Ganymede directly interacts with the corotating jovian plasma, leading to the formation of a mini-magnetosphere which is embedded in the giant magnetosphere of Jupiter. This is the only known case of interaction between two planetary magnetospheres.In the frame of the European space mission JUICE (Jupiter Icy moon Exploration), we investigate this unique interaction with a 3D parallel multi-species hybrid model. This model is based on the CAM-CL algorithm (Matthews 1994) and has been used to study the ionized environments of Titan, Mars and Mercury. In the hybrid formalism, ions are kinetically treated whereas electrons are considered as a zero-inertial fluid to ensure the quasi-neutrality of the plasma. The temporal evolution of the electromagnetic fields is calculated solving Maxwell's equations. The jovian magnetospheric plasma is described as being composed of oxygen and proton ions. The magnetic field of Ganymede, which includes dipolar and induced components (Kivelson et al, 2002), is distorted by its interaction with the Jovian plasma and formed the Alfvén wings. The planetary plasma is described as being composed of O+, with a scale height equal to 125 km. The description of the exosphere is provided by the 3D multi-species collisional exospheric/atmospheric model of Leblanc et al, (2015) and Turc et al. (2014). The ionization of this neutral exosphere by charge exchanges, by electronic impacts, and by reaction with solar photons contributes to the production of planetary plasma. In this model, calculations are performed on a cartesian simulation grid which is refined (down to ~120 km of spatial resolution) at Ganymede, using a multi-grids approach (Leclercq et al., submitted, 2015). Results are compared with Galileo observations obtained during the G1, G2 and G8 flybys

Estudio comparativo de la remoción del hidróxido de calcio, entre irrigación ultrasónica y limas XP-ENDO en raíces con dos conductos

Tesis (Cirujano Dentista)Introducción: En la actualidad existen muchos métodos para remover el hidróxido de calcio de los conductos. Objetivo: Comparar el uso de las limas Xp-Endo Finisher ®, y la irrigación ultrasónica para remover el hidróxido de calcio de las paredes de los conductos, específicamente en dientes que tengan dos conductos en una raíz. Materiales y métodos: Se utilizaron 20 dientes humanos, (específicamente primeros y segundos molares inferiores) que tenían como requisito principal presentar dos conductos radiculares en una misma raíz. Se procedió a la limpieza y sellado de las muestras; a continuación, se llevó a cabo un análisis radiográfico, la preparación de los conductos y posterior medicación. Para luego remover la medicación con dos métodos distintos, 10 dientes (20 conductos) con Xp-Endo Finisher ®, y otros 10, con irrigación ultrasónica pasiva. Luego se procedió a cortar los dientes en sentido vestíbulo-lingual, o coronal, para después analizarlos en un microscopio Olympus CX31 con videocámara ocular conectada al software Micrometrics ®, para hacer la valoración del remanente de hidróxido de calcio en las paredes de los conductos. El análisis estadístico se realizó con el Test Shapiro-Wilk y Test U deMann-Whitney. Resultados: En el tercio cervical no hay evidencia estadísticamente significativa, pero sí en el tercio medio, y especialmente en apical, en los cuales el método de remoción de hidróxido de calcio mediante irrigación ultrasónica pasiva fue más efectivo. 9 Conclusión: Existe diferencia entre ambos métodos de remoción de Ca(OH)2 de las paredes de los conductos.Introduction: There are currently many methods for removing calcium hydroxide from the root canals. Objective: To compare the use of Xp-Endo Finisher ® and passive ultrasonic irrigation (PUI) to remove calcium hydroxide from the surfaces of the root canals, specifically on teeth having two root canals in one root. Materials and methods: Twenty human teeth (specifically first and second lower molars) were used, which had as main requirement to present two root canals in the same root. The samples were cleaned and sealed; a radiographic analysis was done; the preparation of the ducts and subsequent medication were realized. Then, the medication was removed with two different methods, 10 teeth (20 root canals) with Xp-Endo Finisher ®, and another 10, with PUI. Then the teeth were cut in a lingual-vestibular or coronal direction and then analyzed on an Olympus CX31 microscope with an eye-catcher connected to the Micrometrics ® software to evaluate the calcium hydroxide remnant on the surfaces of the root canals. Statistical analysis was performed using the Shapiro-Wilk Test and the U deMann-Whitney Test. Results: In the cervical third there is no statistically significant evidence, but it was significant in the middle third, and especially in the apical, where the method of removal of calcium hydroxide by PUI was more effective. Conclusion: There is a difference between the two methods of removing CA (OH)2 from the surfaces of the root canal

Solar wind charge exchange X-ray emission from Mars Model and data comparison

Aims. We study the soft X-ray emission induced by charge exchange (CX) collisions between solar-wind, highly charged ions and neutral atoms of the Martian exosphere. Methods. A 3D multi species hybrid simulation model with improved spatial resolution (130 km) is used to describe the interaction between the solar wind and the Martian neutrals. We calculated velocity and density distributions of the solar wind plasma in the Martian environment with realistic planetary ions description, using spherically symmetric exospheric H and O profiles. Following that, a 3D test-particle model was developed to compute the X-ray emission produced by CX collisions between neutrals and solar wind minor ions. The model results are compared to XMM-Newton observations of Mars. Results. We calculate projected X-ray emission maps for the XMM-Newton observing conditions and demonstrate how the X-ray emission reflects the Martian electromagnetic structure in accordance with the observed X-ray images. Our maps confirm that X-ray images are a powerful tool for the study of solar wind - planetary interfaces. However, the simulation results reveal several quantitative discrepancies compared to the observations. Typical solar wind and neutral coronae conditions corresponding to the 2003 observation period of Mars cannot reproduce the high luminosity or the corresponding very extended halo observed with XMM-Newton. Potential explanations of these discrepancies are discussed.Comment: 10 pages, 5 figures, accepted for publication in Astron. Astrophysic

Using a virtual cortical module implementing a neural field model to modulate brain rhythms in Parkinson’s disease

We propose a new method for selective modulation of cortical rhythms based on neural field theory, in which the activity of a cortical area is extensively monitored using a two-dimensional microelectrode array. The example of Parkinson’s disease illustrates the proposed method, in which a neural field model is assumed to accurately describe experimentally recorded activity. In addition, we propose a new closed-loop stimulation signal that is both space- and time- dependent. This method is especially designed to specifically modulate a targeted brain rhythm, without interfering with other rhythms. A new class of neuroprosthetic devices is also proposed, in which the multielectrode array is seen as an artificial neural network interacting with biological tissue. Such a bio-inspired approach may provide a solution to optimize interactions between the stimulation device and the cortex aiming to attenuate or augment specific cortical rhythms. The next step will be to validate this new approach experimentally in patients with Parkinson’s disease

Dynamic Martian magnetosphere: Transient twist induced by a rotation of the IMF

International audienceSimulation studies of the Martian environment are usually restricted to stationary situations under various steady conditions of the solar wind and solar radiation. Dynamic transients and their implications have so far attracted little attention although global simulation models can provide valuable insights to understand disagreements between simulations and in situ observations. We make use of a three dimensional multispecies hybrid simulation model to investigate the response of the Martian plasma environment to a sudden rotation of the IMF. The simulation model couples charged and neutral species via three ionisation mechanisms: the absorption of solar extreme ultraviolet radiation, the impact of solar wind electrons, and the charge exchange between ions and neutral atoms. When a rotational discontinuity conveyed by the solar wind reaches the Martian environment the bow shock adapts quickly to the new solar wind conditions in contrast to the induced magnetosphere, especially the magnetic lobes in the wake. Timescales necessary to recover a stationary state can be estimated from such simulations and have some implications for space observations especially in the use of magnetic field proxies and for organizing particle measurements made by a spacecraft like Mars Express without an onboard magnetometer

Influence of the solar EUV flux on the Martian plasma environment

The interaction of the solar wind with the Martian atmosphere and ionosphere is investigated by using three-dimensional, global and multi-species hybrid simulations. In the present work we focus on the influence of the solar EUV flux on the Martian plasma environment by comparing simulations done for conditions representative of the extrema of the solar cycle. The dynamics of four ionic species (H<sup>+</sup>, He<sup>++</sup>, O<sup>+</sup>, O<sub>2</sub><sup>+</sup>), originating either from the solar wind or from the planetary plasma, is treated fully kinetically in the simulation model in order to characterize the distribution of each component of the plasma, both at solar maximum and at solar minimum. The solar EUV flux controls the ionization frequencies of the exospheric species, atomic hydrogen and oxygen, as well as the density, the temperature, and thus the extension of the exosphere. Ionization by photons and by electron impacts, and the main charge exchange reactions are self-consistently included in the simulation model. Simulation results are in reasonable agreement with the observations made by Phobos-2 and Mars Global Surveyor (MGS) spacecraft: 1) the interaction creates a cavity, void of solar wind ions (H<sup>+</sup>, He<sup>++</sup>), which depends weakly upon the phase of the solar cycle, 2) the motional electric field of the solar wind flow creates strong asymmetries in the Martian environment, 3) the spatial distribution of the different components of the planetary plasma depends strongly upon the phase of the solar cycle. The fluxes of the escaping planetary ions are computed from the simulated data and results for solar maximum are compared with estimates based on the measurements made by experiments ASPERA and TAUS on board Phobos-2