In this thesis, we study the effect of diurnally- and seasonally-varying forcing on the global circulation of planetary atmospheres explored within a large parameter space. This work focusses on studying the spacial and spectral energy budgets across a large range of planetary parameters as well as the momentum transfer as a response to diurnal and seasonal effects. We simulate planetary atmospheres using PUMA-GT, a simple GCM co-developed for this work, that is forced by a semi-grey two-band radiative-convective scheme, dissipated by Rayleigh friction and allows for temporally varying insolation. Our parameter regime includes the variation of the planetary rotation rate, frictional timescale in the boundary layer, the thermal inertia of the surface and the atmosphere, as well as the short-wave optical thickness. We calculate the energy transfer in Martian atmosphere to have a reference case of an atmosphere that is subject to very strong seasonal and diurnal variation. For this we present the first Lorenz energy budget calculated from reanalysis data of a non-Earth planet. A comparison between Martian and Earth atmosphere reveals a fundamentally different behaviour of the barotropic conversion term in the global mean. A significant impact of the thermal tide can be discerned in the generation of eddy kinetic energy, especially during global dust storms. Our study of seasonal variation reaffirms previous work that the equatorial super-rotating jet in the slow-rotating regime is arrested for strong seasonal variation. We find a novel explanation as to why the Titan atmosphere is able to maintain super-rotation despite strong surface seasonality; for non-zero short-wave absorption in the atmosphere the mechanism that hinders equatorial super-rotation is weakened. Diurnally-varying forcing can significantly enhance the equatorial super-rotation in cases with non-zero short-wave absorption. In our simulations this enhancement is maintained by a convergence of vertical momentum flux at the equator. Efforts to identify the atmospheric waves involved in this enhancement point towards thermally-excited gravity waves.

Made available in DSpace on 2014-10-09T12:26:24Z (GMT). No. of bitstreams: 0 / Made available in DSpace on 2014-10-09T14:04:20Z (GMT). No. of bitstreams: 0 / Dissertacao (Mestrado) / IPEN/D / Instituto de Pesquisas Energeticas e Nucleares - IPEN-CNEN/SP

Nestes últimos anos, tivemos um aumento no interesse na monitoração dos efeitos da atividade humana sobre a atmosfera e o clima no planeta. O uso de técnicas de sensoriamento remoto têm sido utilizados em diversos estudos, inclusive em estudos relacionados à mudanças globais. Um sistema LIDAR de espalhamento, primeiro deste tipo no Brasil, tem sido usado para fornecer o perfil vertical do coeficiente de retroespalhamento de aerossóis em 532 nm para altitudes de 4 a 6 km acima do nível do mar. Neste estudo, foram utilizados dados coletados no ano de 2005. Estes dados foram correlacionados com dados do fotômetro solar CIMEL e também com dados meteorológicos. Os principais resultados indicaram existir um padrão no comportamento destes dados meteorológicos e a distribuição vertical do coeficiente de extinção obtido através do LIDAR. Em períodos desfavoráveis de dispersão atmosférica, ou seja, elevação da temperatura do ar associado a queda de umidade relativa, aumento da pressão atmosférica e baixa taxa de ventilação, foi possível determinar com boa precisão a altura da Camada Limite Planetária, tanto através do perfil vertical do coeficiente de extinção quanto através da técnica da temperatura potencial. A técnica LIDAR mostrou ser um importante aliado na determinação da estrutura termodinâmica da atmosfera, auxiliando a caracterizar a evolução da CLP ao longo do dia, devido a sua boa resolução espacial e temporal. / In these last years, we had an increase in the interest in the monitoring of the effect of the human activity being on the atmosphere and the climate in the planet. The remote sensing techniques has been used in many studies, also related the global changes. A backscattering lidar system, the first of this kind in Brazil, has been used to provide the vertical profile of the aerosol backscatter coefficient at 532 nm up to an altitude of 4-6 km above sea level. In this study, data has was collected in the year of 2005. These data had been correlated with data of solar photometer CIMEL and also with meteorological data. The main results had indicated to exist a standard in the behavior of these meteorological data and the vertical distribution of the extinction coefficient gotten through LIDAR. In favorable periods of atmospheric dispersion, that is, rise of the temperature of associated air the fall of relative humidity, increase of the atmospheric pressure and low ventilation tax, was possible to determine with good precision the height of the Planetary Boundary Layer, as much through the vertical profile of the extinction coefficient how much through the technique of the vertical profile of the potential temperature. The technique LIDAR showed to be an important tool in the determination of the thermodynamic structure of the atmosphere, assisting to characterize the evolution of the CLP throughout the day, which had its good space and secular resolution.

Made available in DSpace on 2014-10-09T12:26:24Z (GMT). No. of bitstreams: 0 / Made available in DSpace on 2014-10-09T14:04:20Z (GMT). No. of bitstreams: 0 / Nestes últimos anos, tivemos um aumento no interesse na monitoração dos efeitos da atividade humana sobre a atmosfera e o clima no planeta. O uso de técnicas de sensoriamento remoto têm sido utilizados em diversos estudos, inclusive em estudos relacionados à mudanças globais. Um sistema LIDAR de espalhamento, primeiro deste tipo no Brasil, tem sido usado para fornecer o perfil vertical do coeficiente de retroespalhamento de aerossóis em 532 nm para altitudes de 4 a 6 km acima do nível do mar. Neste estudo, foram utilizados dados coletados no ano de 2005. Estes dados foram correlacionados com dados do fotômetro solar CIMEL e também com dados meteorológicos. Os principais resultados indicaram existir um padrão no comportamento destes dados meteorológicos e a distribuição vertical do coeficiente de extinção obtido através do LIDAR. Em períodos desfavoráveis de dispersão atmosférica, ou seja, elevação da temperatura do ar associado a queda de umidade relativa, aumento da pressão atmosférica e baixa taxa de ventilação, foi possível determinar com boa precisão a altura da Camada Limite Planetária, tanto através do perfil vertical do coeficiente de extinção quanto através da técnica da temperatura potencial. A técnica LIDAR mostrou ser um importante aliado na determinação da estrutura termodinâmica da atmosfera, auxiliando a caracterizar a evolução da CLP ao longo do dia, devido a sua boa resolução espacial e temporal. / Dissertacao (Mestrado) / IPEN/D / Instituto de Pesquisas Energeticas e Nucleares - IPEN-CNEN/SP

HAT-P-30-WASP-51b is a hot-Jupiter exoplanet that orbits an F star every 2.8106 days at a distance of 0.0419 AU. Using the Spitzer Space Telescope in 2012 (Spitzer Program Number 70084) we observed two secondary eclipses at 3.6 and 4.5 μm. We present eclipse-depth measurements of 0.177 ± 0.018 % and 0.247 ± 0.024 % and estimate the infrared brightness temperatures to be 1990 ± 110 K and 2080 ± 130 K for these two channels, respectively, from an analysis using our Photometry for Orbits, Eclipses, and Transits (POET) pipeline. These may be grazing eclipses. We also refine its orbit using our own secondary-eclipse measurements in combination with radial- velocity and transit observations from both professional and amateur observers. Using only the phase of our secondary eclipses, we can constrain e cos(ω) where e is the orbital eccentricity and ω is the argument of periastron to 0.0058 ± 0.00094. This is the component of eccentricity in the plane of view,. This small but non-zero eccentricity is independent of the effects that stellar tides have on radial-velocity data. When including radial velocity data in our model, our Markov chain finds an e cos(ω) of 0.0043 ± 0.0007. We constrain the atmospheric temperature profile using our Bayesian Atmospheric Radiative Transfer code (BART), a large lower bound (700 km) for the scale height, and the potential for high quality transit spectroscopy observations.

The object of this research program has been to provide a baseline for microwave remote sensing of ammonia and water vapor in the atmosphere of Jupiter through laboratory measurements of their microwave absorption properties. Jupiter is not only the largest planet in our solar system, but one of the most interesting and complex. Despite a handful of spacecraft missions and many astronomical measurements, much of Jupiter s atmospheric dynamics and composition remain a mystery. Although constraints have been formed on the amount of certain gases present, the global abundances and distributions of water vapor (H2O) and ammonia (NH3) are relatively unknown. Measurements of H2O and NH3 in the Jovian atmosphere to hundreds of bars of pressure are best accomplished via passive microwave emission measurements. For these measurements to be accurately interpreted, however, the hydrogen and helium pressure-broadened microwave opacities of H2O and NH3 must be well characterized, a task that is very difficult if based solely on theory and limited laboratory measurements. Therefore, accurate laboratory measurements have been taken under a broad range of conditions that mimic those of the Jovian atmosphere. These measurements, performed using a newly redesigned high-accuracy system, and the corresponding models of microwave opacity that have been developed from them comprise the majority of this work. The models allow more accurate retrievals of H2O and NH3 abundances from previous as well as future missions to Jupiter and the outer planets, such as the NASA New Frontiers class Juno mission scheduled for launch in 2011. This information will enable a greater understanding of the concentration and distribution of H2O and NH3 in the Jovian atmosphere, which will reveal much about how Jupiter and our solar system formed and how similar planets could form in other solar systems, even planets that may be hospitable to life.

In order to fully understand the role methane (CH₄) plays in the microwave emission spectra of the deep atmospheres of the outer planets, over 280 laboratory measurements of the opacity of ammonia in a methane environment have been made in the 5-20 cm wavelength range. All opacity measurements were made with either 100 or 200 mbars of ammonia and with 1 to 3 bars of added methane in the 330-450K temperature range. A formalism for the absorptivity of ammonia broadened by methane has now been developed and had been applied to the Hanley et al. (Icarus, v. 202, 2009) model for the opacity of ammonia. Due to methane's relatively low abundance at Jupiter (~0.2% by volume), its effect on the microwave spectrum which will be observed by the Juno MWR (Microwave Radiometer) will be minimal. However, these experimental results will significantly improve the understanding of the microwave emission spectrum of Uranus and Neptune where methane plays a more dominant role.

Cette thèse se penche sur la propagation d’ondes au sein du système coupléTerre-océan-atmosphère. La compréhension de ces phénomènes a une importance majeure pour l’étude de perturbations sismiques et d’explosions atmosphériques notamment dans le cadre de missions spatiales planétaires. Les formes d’ondes issues du couplage fluide-solide permettent d’obtenir de précieuses informations sur la source du signal ou les propriétés des milieux de propagation. On développe donc deux outils numériques d’ordre élevé pour la propagation d’ondes acoustiques et de gravité. L'u en différences finies et se concentre sur le milieu atmosphérique et la propagation d’ondes linéaires dans un milieu stratifié visqueux et avec du vent. Cette méthode linéaire est validée par des solutions quasi-analytiques reposant sur les équations de dispersion dans une atmosphère stratifiée. Elle est aussi appliquée à deux cas d’études : la propagation d’ondes liée à l’impact d’une météorite à la surface de Mars (mission NASA INSIGHT), et la propagation d’ondes atmosphériques liées au tsunami de Sumatra en 2004. La seconde méthode résout la propagation non-linéaire d’ondes gravito-acoustiques dans une atmosphère couplée, avec topographie, à la propagation d’ondes élastiques dans un solide visco-élastique. Cette méthode repose sur sur le couplage d’une formulation en éléments finis discontinus, pour résoudre les équations de Navier-Stokes la partie fluide, par éléments finis continus pour résoudre les équations de l’élastodynamique dans la partie solide. Elle a été validée grâce à des solutions analytiques ainsi que par des comparaisons avec les résultats de la méthode par différences finies. / This thesis deals with the wave propagation problem within the Earth-ocean-atmosphere coupled system. A good understanding of the these phenomena has a major importance for seismic and atmospheric explosion studies, especially for planetary missions. Atmospheric wave-forms generated by explosions or surface oscillations can bring valuable information about the source mechanism or the properties of the various propagation media. We develop two new numerical full-wave high-order modeling tools to model the propagation of acoustic and gravity waves in realistic atmospheres. The first one relies on a high-order staggered finite difference method and focus only on the atmosphere. It enables the simultaneous propagation of linear acoustic and gravity waves in stratified viscous and windy atmosphere. This method is validated against quasi-analytical solutions based on the dispersion equations for a stratified atmosphere. It has also been employed to investigate two cases : the atmospheric propagation generated by a meteor impact on Mars for the INSIGHT NASA mission and for the study of tsunami-induced acoutic and gravity waves following the 2004 Sumatra tsunami. The second numerical method resolves the non-linear acoustic and gravity wave propagation in a realistic atmosphere coupled, with topography, to the elastic wave propagation in a visco-elastic solid. This numerical tool relies on a discontinuous Galerkin method to solve the full Navier-Stokes equations in the fluid domain and a continuous Galerkin method to solve the elastodynamics equations in the solid domain. It is validated against analytical solutions and numerical results provided by the finite-difference method.

Made available in DSpace on 2014-10-09T12:42:00Z (GMT). No. of bitstreams: 0 / Made available in DSpace on 2014-10-09T14:04:50Z (GMT). No. of bitstreams: 0 / Dissertação (Mestrado) / IPEN/D / Instituto de Pesquisas Energeticas e Nucleares - IPEN-CNEN/SP

Made available in DSpace on 2014-10-09T12:42:00Z (GMT). No. of bitstreams: 0 / Made available in DSpace on 2014-10-09T14:04:50Z (GMT). No. of bitstreams: 0 / Esta dissertação aborda um estudo sobre algoritmos matemáticos (Método da Variância, Método das Imagens, Método do Gradiente (MG), WCT - Wavelet Covariance Transform), os quais possibilitam a obtenção da altura máxima da Camada Limite Planetária (CLP) a partir de dados fornecidos por um sistema lidar. Em um primeiro momento será descrita a CLP e as suas principais variáveis, assim como também os métodos juntamente com os seus pontos positivos e negativos. Em seguida serão abordadas duas situações de medida: a primeira consiste em um estudo de casos realizado na cidade de Vitória-ES, para o qual foram escolhidas três situações típicas (calmaria, presença de subcamadas de aerossóis e/ou camadas de nuvens e turbulência) em que os métodos foram: testados, comparados entre si, com a análise visual do perfil e o BRN (Bulk Richardsons Number); a segunda situação aborda uma medida feita na cidade de São Paulo-SP durante um período de 12 horas contínuas, sendo o grande diferencial deste experimento, o lançamento de radiossondas dentro de intervalos de 3 horas, isso aliado a utilização de modelagem WRF (Weather Research Forecasting) permitiu uma maior comparação e validação dos dados. A partir dos estudos de casos foi possível observar que com o aumento da complexidade do perfil apresentado pela atmosfera, há um decréscimo na qualidade dos resultados apresentados pelos métodos e um aumento no tempo de processamento, já que há necessidade de um maior refinamento nos parâmetros que serão utilizados. Nas situações de \"calmaria\"o perfil da atmosfera se mostra mais simplificado, o que facilita a escolha de qual método utilizar, sendo que com exceção da Variância, todos os outros métodos forneceram resultados satisfatórios. Para o caso de \"presença de subcamadas de aerossóis e/ou nuvens\"a qualidade dos resultados apresentados pelos métodos decai sendo exceção da Variânci, uma vez que esta passa a apresentar resultados mais próximos do esperado devido ao aumento na complexidade do sinal lidar. Na situação caracterizada como \"turbulência\", todos os métodos passam a apresentar maiores dificuldades para detectar corretamente a CLP, sendo que o WCT se mostra o mais robusto, porém exige uma complexa escolha de parâmetros, demandando um alto tempo de processamento. Na medida de 12 horas contínuas todos os métodos conseguem representar satisfatoriamente a ascensão e o decaimento da CLP, ficando as maiores divergências para o meio do dia, principalmente quando há dispersão dos aerossóis gerando atenuação no sinal, com isso os métodos mais sensíveis (MG e Método das Imagens) passam a apresentar várias oscilações, dificultando a detecção do topo da CLP. As análises realizadas permitiram observar as vantagens e desvantagens de cada método, assim como descobrir qual possui o uso mais indicado para cada cenário meteorológico, sendo o algoritmo WCT o mais robusto em todas as situações apresentadas. / Dissertação (Mestrado) / IPEN/D / Instituto de Pesquisas Energeticas e Nucleares - IPEN-CNEN/SP