Our knowledge of stellar magnetic fields relies almost entirely on circular polarization observations, which has historically limited our understanding of the stellar magnetic field topologies. Recently, it has become possible to obtain phase-resolved high-resolution spectropolarimetric observations in all four Stokes parameters for early-type magnetic stars. Interpretation of such observations with the Magnetic Doppler imaging technique has uncovered a new, previously unknown, level of complexity of surface stellar magnetic fields. This new insight is critical for understanding the origin, evolution and structure of magnetic fields in early-type stars. In this study we observed the magnetic, chemically peculiar Ap stars HD 24712 (DO Eri, HR 1217) and HD 125248 (CS Vir, HR 5355) in all four Stokes parameters with the HARPSpol spectropolarimeter at the ESO 3.6-m telescope. The resulting spectra have high signal-to-noise ratio and superb resolving power, by far surpassing the quality of any existing stellar Stokes parameter observations. We studied variation of the spectrum and magnetic observables of HD 24712 as a function of rotational phase (paper I). In the subsequent magnetic Doppler imaging investigation of this star, we interpreted the phase-resolved Stokes line profile observations (paper II). This analysis showed that HD 24712, unlike more massive Ap stars studied in all four Stokes parameters, has a dominant dipolar field component with a negligible contribution of small-scale magnetic structures. Simultaneously with magnetic mapping we derived surface abundance distributions of Fe, Nd, Na, and Ca. Building upon the technique of Magnetic Doppler imaging, we developed the first three-dimensional abundance inversion code and applied it to reconstruct the abundance distributions of Fe and Ca in three dimensions in the atmosphere of HD 24712 (paper III). We also performed Magnetic Doppler imaging analysis of the spectropolarimetric observations of HD 125248 (paper IV). The reconstructed detailed maps of the surface abundance distribution and magnetic field topology of HD 125248 revealed a magnetic field with significant deviations from the canonical dipolar field geometry, and strong surface abundance inhomogeneities for Cr and several rare earth elements. We assessed our inversion results in the context of magnetic Doppler imaging studies of other magnetic, chemically peculiar Ap stars and latest theoretical research on the evolution and stability of magnetic fields in radiative stellar interiors. Our analysis suggests that old or less massive Ap stars have predominantly dipolar magnetic fields while more massive or younger stars exhibit more complicated field topologies. We also compared our three-dimensional chemical abundance maps of HD 24712 to the predictions of theoretical atomic diffusion calculations in magnetized stellar atmospheres, generally finding a lack of agreement between theory and observations.

No description available.

We present results from the first observations of the Hubble Space Telescope (HST) Panchromatic Comparative Exoplanet Treasury program for WASP-101b, a highly inflated hot Jupiter and one of the community targets proposed for the James Webb Space Telescope (JWST) Early Release Science (ERS) program. From a single HST Wide Field Camera 3 observation, we find that the near-infrared transmission spectrum of WASP-101b contains no significant H2O absorption features and we rule out a clear atmosphere at 13 sigma. Therefore, WASP-101b is not an optimum target for a JWST ERS program aimed at observing strong molecular transmission features. We compare WASP-101b to the well-studied and nearly identical hot Jupiter WASP-31b. These twin planets show similar temperature-pressure profiles and atmospheric features in the near-infrared. We suggest exoplanets in the same parameter space as WASP-101b and WASP-31b will also exhibit cloudy transmission spectral features. For future HST exoplanet studies, our analysis also suggests that a lower count limit needs to be exceeded per pixel on the detector in order to avoid unwanted instrumental systematics.

To date more than 1500 exoplanets have been discovered. A large number of these are hot Jupiters, Jupiter-sized planets orbiting < 0.1 au from their parent stars, due to limitations in observational techniques making them easier to detect than smaller planets in wider orbits. This is also, for the same reasons, the class of exoplanets with the most observational constraints. Due to the very large interaction between these planets and their parent stars they are believed to be tidally locked, causing a large temperature contrast between the permanently hot day side and colder night side. There are still many open questions about these planets. Many are observed to have inflated radii, i.e. the observed radius is larger for a given mass than evolutionary models predict. A mechanism that can transport some of the stellar heating into the interior of the planet may be able to explain this. The presence of hazes or clouds has been inferred on some planets, but their composition and distribution remain unknown. According to chemical equilibrium models TiO and VO should be present on the day side of the hottest of these planets, but these molecules have not yet been detected. Cold traps, where these molecules condense out on the night side, have been suggested to explain this. The efficiency of the heat redistribution from the day side to the night side has been found to vary significantly between different planets; the mechanism behind this is still unknown. To begin to answer many of these questions we need models capturing the three-dimensional nature of the atmospheres of these planets. General circulation models (GCMs) do this by solving the equations of fluid dynamics for the atmosphere coupled to a radiative transfer scheme. GCMs have previously been applied to several exoplanets, but many solve simplified fluid equations (shallow water or primitive equations) or highly parametrised radiation schemes (temperature-forcing, gray or band-averaged opacities). We here present an adaptation of the Met Office Unified Model (UM), a GCM used for weather predictions and climate studies for the Earth, to hot Jupiters. The UM solves the full 3D Euler equations for the fluid, and the radiation scheme uses the two-stream approximation and correlated-k method, which are state of the art for both Earth and exoplanet GCMs. This makes it ideally suited for the study of hot Jupiters. An important part of this work is devoted to the adaptation of the radiation scheme of the UM to hot Jupiters. This includes calculation of opacities for the main absorbers in these atmospheres from state-of-the-art high temperature line lists, the calculation of k-coefficients from these opacities, and making sure all aspects of the scheme perform satisfactorily at high temperatures and pressures. We have tested approximations made in previous works such as the two-stream approximation, use of band-averaged opacities and different treatments of gaseous overlap. Uncertainties in current models, such as the lack of high temperature line broadening parameters for these atmospheres, are discussed. We couple the adapted radiation scheme to the UM dynamical core, which has been tested independently. Our first application is devoted to one of the most well-observed hot Jupiters, HD 209458b. Differences between previous modelling works and our model are discussed, and we compare results from the full coupled model with results obtained using a temperature-forcing scheme. We have also developed a tool to calculate synthetic phase curves, and emission and transmission spectra from the output of our 3D model. This enables us to directly compare our model results to observations and test the effect of various parameters and model choices on observable quantities.

Over a large range of equilibrium temperatures, clouds shape the transmission spectrum of hot Jupiter atmospheres, yet their composition remains unknown. Recent observations show that the Kepler light. curves of some hot Jupiters are asymmetric: for the hottest planets, the light. curve peaks before secondary eclipse, whereas for planets cooler than similar to 1900 K, it peaks after secondary eclipse. We use the thermal structure from 3D global circulation models to determine the expected cloud distribution and Kepler light. curves of hot Jupiters. We demonstrate that the change from an optical light. curve dominated by thermal emission to one dominated by scattering (reflection) naturally explains the observed trend from negative to positive offset. For the cool planets the presence of an asymmetry in the Kepler light curve is a telltale sign of the cloud composition, because each cloud species can produce an offset only over a narrow range of effective temperatures. By comparing our models and the observations, we show that the cloud composition of hot Jupiters likely varies with equilibrium temperature. We suggest that a transition occurs between silicate and manganese sulfide clouds at a temperature near 1600 K, analogous to the L/T transition on brown dwarfs. The cold trapping of cloud species below the photosphere naturally produces such a transition and predicts similar transitions for other condensates, including TiO. We predict that most hot Jupiters should have cloudy nightsides, that partial cloudiness should be common at the limb, and that the dayside hot spot should often be cloud-free.

We present Spitzer/Infrared Array Camera Ch1 and Ch2 monitoring of six brown dwarfs during eight different epochs over the course of 20 months. For four brown dwarfs, we also obtained simulataneous Hubble Space Telescope (HST)/WFC3 G141 grism spectra during two epochs and derived light curves in five narrowband filters. Probing different pressure levels in the atmospheres, the multiwavelength light curves of our six targets all exhibit variations, and the shape of the light curves evolves over the timescale of a rotation period, ranging from 1.4 to 13 hr. We compare the shapes of the light curves and estimate the phase shifts between the light curves observed at different wavelengths by comparing the phase of the primary Fourier components. We use state-of-the-art atmosphere models to determine the flux contribution of different pressure layers to the observed flux in each filter. We find that the light curves that probe higher pressures are similar and in phase, but are offset and often different from the light curves that probe lower pressures. The phase differences between the two groups of light curves suggest that the modulations seen at lower and higher pressures may be introduced by different cloud layers.

Hydrogen gas evaporating from the atmosphere of the hot-Neptune GJ436b absorbs over 50% of the stellar Lya emission during transit. Given the planet's atmospheric composition and energy-limited escape rate, this hydrogen outflow is expected to entrain heavier atoms such as C and O. We searched for C and Si in the escaping atmosphere of GJ436b using far-ultraviolet Hubble Space Telescope COS G130M observations made during the planet's extended H I transit. These observations show no transit absorption in the C II 1334,1335 angstrom and Si III 1206 angstrom lines integrated over [-100, 100] km s(-1), imposing 95% (2 sigma) upper limits of 14% (C II) and 60% (Si III) depth on the transit of an opaque disk and 22% (C II) and 49% (Si III) depth on an extended highly asymmetric transit similar to that of H I Ly alpha. C+ is likely present in the outflow according to a simulation we carried out using a spherically symmetric photochemical-hydrodynamical model. This simulation predicts an similar to 2% transit over the integrated bandpass, consistent with the data. At line center, we predict the C II transit depth to be as high as 19%. Our model predicts a neutral hydrogen escape rate of 1.6 x 10(9) g s(-1) (3.1 x 10(9) g s(-1) for all species) for an upper atmosphere composed of hydrogen and helium.

We present an outline of basic assumptions and governing structural equations describing atmospheres of sub-stellar mass objects, in particular the extrasolar giant planets and brown dwarfs. Although most of the presentation of the physical and numerical background is generic, details of the implementation pertain mostly to the code COOLTLUSTY. We also present a review of numerical approaches and computer codes devised to solve the structural equations, and make a critical evaluation of their efficiency and accuracy.

As propriedades de superfícies de pós cerâmicos desempenham um papel importante na produção de dispositivos de alta qualidade, elevado desempenho e confiabilidade. Muitas dessas propriedades estão relacionadas a interações com o meio em que o material esta presente. Um exemplo, são materiais cerâmicos utilizados em sensores de gases. A perovisquita BaSnO3 (estanato de bário) é um de material cerâmico promissor a sensor de gás. Neste sentido, a proposta do presente trabalho consistiu em realizar a síntese do composto BaSnO3 por reação no estado sólido e preparar cerâmicas com o objetivo de estudar suas propriedades estruturais, microestruturais e seu comportamento elétrico em função da atmosfera. As amostras foram caracterizadas utilizando-se as técnicas de termogravimetria, calorimetria exploratória diferencial, difratometria de raios x, microscopia eletrônica de varredura, dilatometria e espectroscopia de impedância. Para a produção do BaSnO3 foram utilizadas duas metodologias de síntese. A primeira, chamada de rota 1, a preparação foi realizada a partir da mistura direta dos pós precursores, sem aquecimento prévio. A segunda metodologia, denominada rota 2, os pós precursores foram submetidos a um aquecimento separadamente antes da mistura e síntese. Os resultados obtidos utilizando a rota 1 mostraram a presença de fases secundárias (SnO2 e BaCO3) ao material pretendido, além da formação de fase líquida durante o processo de sinterização das cerâmicas. Contudo, os resultados obtidos com o procedimento adotado na rota 2 mostraram apenas a presença da fase desejada e ausência de fase líquida durante a sinterização. Com o objetivo de assegurar que a presença de fases secundárias na rota 1 e a fase líquida observadas nas microestruturas foram devido a presença de água adsorvida nos pós precursores, corpos cerâmicos `a verde produzidos pela rota 2 foram submetidos a imersão em água por aproximadamente 10 horas antes da sinterização. Este procedimento não resultou no aparecimento de fases secundárias, como era esperado, porém verificou-se a formação de fase líquida durante o processo de sinterização. As cerâmicas assim processadas apresentaram menor densidade relativa e maior tamanho médio de grão. Para a caracterização elétrica das cerâmicas foram utilizados as seguintes atmosferas: ar, em condição de pressão distinta, argônio contendo 5% de hidrogênio e argônio contendo 15% de hidrogênio. Os resultados mostraram que o estanato de bário apresenta significativa sensibilidade relativa da condutividade elétrica para as atmosferas estudadas a temperaturas acima de 100oC. / The surface properties of ceramic powders play an important role in the production of devices of high quality, high performance and reliability. Many of these properties are related to interactions with the environment. One example, ceramics are used in gas sensor devices. A ceramic material that has been reported as promising gas sensor is perovskite BaSnO3 (barium stannate). In this work we performed the synthesis of the BaSnO3 compound by solid state reaction to study its structural properties, microstructure and electrical behavior in function of atmosphere. The samples were characterized by thermogravimetry, differential scanning calorimetry, x-ray diffraction, scanning electron microscopy, dilatometry and impedance spectroscopy. For the production of BaSnO3 used two methods of synthesis. the first method, called route 1, the preparation was performed directly from the mixing of powder precursors. The second, named as route 2, the precursor powders were subjected to heating separately before mixing. The results obtained using the route 1 showed the presence of secondary phases (SnO2 and BaCO3) and the formation of liquid phase during sintering of the ceramics. The results obtained with the procedure adopted in the route 2 showed only the presence of the desired (BaSnO3) phase and no liquid phase during sintering. In order to investigate what the effects caused by the water adsorption by perovskite BaSnO3, the green-ceramic bodies produced by route 2 were submitted to immersion in water prior to sintering. This procedure did not result in the appearance of secondary phases, but was verified the presence of the liquid phase, and the ceramics showed lower density and larger average grain size. For the electrical characterization we used the following atmospheres: vacuum, air, argon containing 5% hydrogen and argon containing 15% hydrogen. The results showed that the barium stannate shows a significant sensitivity to the conductivity in the studied atmospheres at temperatures above 100oC.

As propriedades de superfícies de pós cerâmicos desempenham um papel importante na produção de dispositivos de alta qualidade, elevado desempenho e confiabilidade. Muitas dessas propriedades estão relacionadas a interações com o meio em que o material esta presente. Um exemplo, são materiais cerâmicos utilizados em sensores de gases. A perovisquita BaSnO3 (estanato de bário) é um de material cerâmico promissor a sensor de gás. Neste sentido, a proposta do presente trabalho consistiu em realizar a síntese do composto BaSnO3 por reação no estado sólido e preparar cerâmicas com o objetivo de estudar suas propriedades estruturais, microestruturais e seu comportamento elétrico em função da atmosfera. As amostras foram caracterizadas utilizando-se as técnicas de termogravimetria, calorimetria exploratória diferencial, difratometria de raios x, microscopia eletrônica de varredura, dilatometria e espectroscopia de impedância. Para a produção do BaSnO3 foram utilizadas duas metodologias de síntese. A primeira, chamada de rota 1, a preparação foi realizada a partir da mistura direta dos pós precursores, sem aquecimento prévio. A segunda metodologia, denominada rota 2, os pós precursores foram submetidos a um aquecimento separadamente antes da mistura e síntese. Os resultados obtidos utilizando a rota 1 mostraram a presença de fases secundárias (SnO2 e BaCO3) ao material pretendido, além da formação de fase líquida durante o processo de sinterização das cerâmicas. Contudo, os resultados obtidos com o procedimento adotado na rota 2 mostraram apenas a presença da fase desejada e ausência de fase líquida durante a sinterização. Com o objetivo de assegurar que a presença de fases secundárias na rota 1 e a fase líquida observadas nas microestruturas foram devido a presença de água adsorvida nos pós precursores, corpos cerâmicos `a verde produzidos pela rota 2 foram submetidos a imersão em água por aproximadamente 10 horas antes da sinterização. Este procedimento não resultou no aparecimento de fases secundárias, como era esperado, porém verificou-se a formação de fase líquida durante o processo de sinterização. As cerâmicas assim processadas apresentaram menor densidade relativa e maior tamanho médio de grão. Para a caracterização elétrica das cerâmicas foram utilizados as seguintes atmosferas: ar, em condição de pressão distinta, argônio contendo 5% de hidrogênio e argônio contendo 15% de hidrogênio. Os resultados mostraram que o estanato de bário apresenta significativa sensibilidade relativa da condutividade elétrica para as atmosferas estudadas a temperaturas acima de 100oC. / The surface properties of ceramic powders play an important role in the production of devices of high quality, high performance and reliability. Many of these properties are related to interactions with the environment. One example, ceramics are used in gas sensor devices. A ceramic material that has been reported as promising gas sensor is perovskite BaSnO3 (barium stannate). In this work we performed the synthesis of the BaSnO3 compound by solid state reaction to study its structural properties, microstructure and electrical behavior in function of atmosphere. The samples were characterized by thermogravimetry, differential scanning calorimetry, x-ray diffraction, scanning electron microscopy, dilatometry and impedance spectroscopy. For the production of BaSnO3 used two methods of synthesis. the first method, called route 1, the preparation was performed directly from the mixing of powder precursors. The second, named as route 2, the precursor powders were subjected to heating separately before mixing. The results obtained using the route 1 showed the presence of secondary phases (SnO2 and BaCO3) and the formation of liquid phase during sintering of the ceramics. The results obtained with the procedure adopted in the route 2 showed only the presence of the desired (BaSnO3) phase and no liquid phase during sintering. In order to investigate what the effects caused by the water adsorption by perovskite BaSnO3, the green-ceramic bodies produced by route 2 were submitted to immersion in water prior to sintering. This procedure did not result in the appearance of secondary phases, but was verified the presence of the liquid phase, and the ceramics showed lower density and larger average grain size. For the electrical characterization we used the following atmospheres: vacuum, air, argon containing 5% hydrogen and argon containing 15% hydrogen. The results showed that the barium stannate shows a significant sensitivity to the conductivity in the studied atmospheres at temperatures above 100oC.