GLOBAL ATMOSPHERE

Author: CONANGLA TRIVIÑO LAURA.
Year: 2004.
University: BARCELONA [www.ub.es].
Place of defense: FACULTAT DE FÍSICA.
Place of preparation: FACULTA DE FÍSICA - UNIVERSITAT DE BARCELONA.

Author: GARCIA MELENDO ENRIQUE.
Year: 2004.
University: POLITÉCNICA DE CATALUÑA [www.upc.edu].
Place of defense: AULA TELEENSENYAMENT. EDIFICI B3. CAMPUS NORD.
Place of preparation: EDIFICI B4 DESPATX 108 NORD.

Summary: The overall objective of this dissertation is to study the atmosphere joviana to provide evidence to suggest whether the origin of the global circulation, observed at the level of the ceiling of clouds, is originally from deep or superficial as predicting the two major competing models: general circulation deep, and global circulation surface. First we study the stability of the zonal winds to observe possible variability, as the deep circulation models predict a high stability over time, while the surface give way to possible variations due to various reasons such as seasonality. In this first part of the work were used archival images taken by the Hubble Space Telescope between 1995 and 2000 at various wavelengths to study the stability of the zonal winds. This study discovered three new jet streams at high latitudes, two located 63N and 68N and another 62S. Globally it is shown that between 1995 and 2000 there were no significant changes in the structure of the zonal flow means of Jupiter. These results were fully corroborated by the results obtained by the Cassini probe on its overflight of Jupiter during 2000-2001 (Porco et al. 2003). In a second phase of the thesis is selected as a particular region of North Temperate study Band (NTB) located in volume in the jet stream to 24N. The NTB suffered a rash of nature convecting in 1991 as temporal evolution allows you to limit clear-cut numerical models better than most other regions of the planet. The final stage of development of the disturbance is a series of vortices long life (-10 years), whose dynamic properties are studied in detail in connection with the jet stream in to 24N on which they are located. The study of the vorticity of the vortices serves to verify that it is similar to the vorticity environment, suggesting that their origin is probably linked to a hydrodynamic instability of origin, without any input of energy from other sources. These results into the vortex of the long life and its evolution from a disturbance in the jet stream to 24N, objects designed to establish a numerical model that can give us more details about how the structure of the atmosphere joviana by beneath the roof visible cloud. Finally, it provides a model to simulate atmospheric as precisely as possible the morphological evolution of the eruption of the NTB until the onset of long-lived vortices (García-Melendo et al. 2005). It employs EPIC (Dowling 1998), a numerical model that solves the equations of motion in Isentropic coordinates, that is, where the elements of fluid move so adiabática. The two most important parameters of the model-free atmosphere are the thermal structure of the atmosphere and the vertical wind profile uv (p). The main conclusion to be derived from simulations is that the behavior of long-term disruption of the NTB, it can only be reproduced for a pequeílo subset of zonal and vertical profiles of all those who can characterize the current jet in that region. Starting from a speed of 180 ms-l level clouds visible ammonia, the best model indicates that the maximum speed of the jet stream in due until 210 ms-la the growing pressure l bar, and then grow more slowly up the 240 ms-I level 6 bars with ulz -17 ms-l by height scale. The vertical profile so obtained is consistent with the measured by the Galileo probe to 7N (Atkinson et al. 1998), and with the hipóte 8 sis of q 2ca ue overall wind speed increases with depth.

Author: González Galindo Francisco.
Year: 2005.
University: GRANADA [www.ugr.es].
Place of defense: Universidad de Granada.
Place of preparation: Instituto de Astrofísica de Andalucía, CSIC.

Summary: This dissertation presents a series of studies of the upper atmosphere of Mars made with theoretical models. The introduction summarizes the scientific research milestones that have marked the knowledge of the physical, chemical and geological Mars, starting with the first telescopic explorations and even the recent space missions. The latter have allowed us to obtain a detailed knowledge whenever the Martian atmosphere, as summarize the second part of this introduction. In a third party, described the European Mars General Circulation Model, the main tool used in this work. Finally, it outlines the motivations and objectives of this work. The second chapter describes the process of developing a model 1-D of the upper atmosphere of Mars. The main physical processes governing the state of the Martian upper atmosphere are analyzed in detail, since theory and numerical simulation, until the results of each mechanism separately. We present some results of coupling between all of them. The third chapter presents the schemes quick calculation based on detailed models described above, for the heating and UV photochemistry. The schedule for the heating UV is based on a division of the spectrum in 36 subintervals and a tabulation of the coefficients fotoabsorción depending on the column absorbents Martians. It includes fixes for the variation of solar flux during the solar cycle of 11 years, and the variation of the cross section of CO2 with temperature. For photochemistry, the scheme is based on the approximation of photochemical balance for the three compounds with a lifetime shorter. In both cases shows the behavior of these schemes rapid compared with detailed calculations described above. In the fourth chapter we studied the results of the nominal length termosférica of EMGCM, paying particular attention to the thermal structure and analyzing the relative importance of the radiative and dynamical processes. Desvelamos an important acoplo between the low and high thermosphere. They also studied the seasonal variability and with the solar cycle in temperatures, comparing with previous results from other models and observations. Summarized in the fifth chapter validation of the extension termosférica of EMGCM: susceptibility testing and comparison with other models. The first allows us to study if the results meet expectations physical, and while we show the dependence of the results compared to changes in input parameters. In particular, we studied the effects on the efficiency of varying temperatures warming and the rate of UV-energizing colisional CO2. Comparisons with the MTGCM show differences due to the implementation of different parameterization used for the study of cooling broadcasts in 15 micron CO2. Once the implementation of this process is similar in the two models, both of which use the same solar UV flux, the difference in temperature is about 10 K value close to the inherent variability of the models. After the summary, conclusions and further work will include a series of appendices in which summarizes various numerical methods and physical: the method of finite differences, and the radiative transport method for resolving equations photochemical. It also summarizes some results, as production and losses of all compounds, the calculation of the energy of chemical reactions and the boards of photo-dissociation coefficients. Lastly, summarizes the main characteristics of the different General Circulation Models of the Martian atmosphere.

Author: PÉREZ HOYOS SANTIAGO.
Year: 2005.
University: PAÍS VASCO [www.ehu.es].
Place of defense: ESCUELA TÉCNICA SUPERIOR DE INGENIERÍA.
Place of preparation: ESCUELA TÉCNICA SUPERIOR DE INGENIERÍA.

Summary: This thesis presents an analysis of the vertical structure of clouds, fog and aerosols in the atmosphere of Saturn. This imagery has been used for the Hubble Space Telescope between the years 1994 and 2004. The comments of the variation of the absolute reflectivity of the planet from the ultraviolet to the near infrared has been reproduced using a radiative transport code that lets us know the vertical distribution of fog between 1Â º mbar and 2 bar pressure. The model can explain the latitudinal and temporal differences observed, as well as the vertical structure of elements used as tracers of winds in other work (both at the time Voyager 1979-81 and in the HST 1996-2004), especially in the area of the equatorial planet, which has detected substantial variations in height and winds at the time. The study is complemented by an analysis of the penetration of solar radiative flux in the atmosphere mean and calculating rates of warming occurred at different atmospheric levels.