The Dynamics in the Upper Atmospheres of Mars and Titan.

Planetary Atmospheres;Mars and Titan;Thermosphere-Ionosphere;Atmospheric;Oceanic and Space Sciences;Science;Space and Planetary Physics

Bell, Jared MichealWaite, Jr Jack ;

University of Michigan

关键词: Planetary Atmospheres;    Mars and Titan;    Thermosphere-Ionosphere;    Atmospheric;    Oceanic and Space Sciences;    Science;    Space and Planetary Physics;   

Others  :  https://deepblue.lib.umich.edu/bitstream/handle/2027.42/60693/jmbell_1.pdf?sequence=1&isAllowed=y

瑞士|英语

来源: The Illinois Digital Environment for Access to Learning and Scholarship

【 摘 要 】

This thesis explores the dynamics of two terrestrial bodies: Mars and Titan. At Mars, the coupled Mars General Circulation Model - Mars Thermospheric General Circulation Model (MGCM-MTGCM) is employed to investigate the phenomenon known as Mars winter polar warming. At Titan, a new theoretical model, the Titan Global Ionosphere-Thermosphere Model (T-GITM), is developed, based on the previous modeling work of Ridley et al. [2006]. Using this new model, three separate numerical studies quantify the impacts of solar cycle, seasons, and lower boundary zonal winds on the Titan thermosphere structure and dynamics. At Mars, this thesis investigates winter polar warming through three major studies: (1) a systematic analysis of vertical dust mixing in the lower atmosphere and its impact upon the dynamics of the lower thermosphere (100 − 130 km), (2) an interannual investigation utilizingthree years of lower atmosphere infrared (IR) dust optical depth data acquired by the Thermal Emission Spectrometer (TES) instrument on board Mars Global Surveyor (MGS), and finally (3) a brief study of the MTGCM’s response to variations in upward propagating waves and tides from the lower atmosphere. Ultimately, this investigation suggests that an interhemispheric summer-to-winter Hadley circulation, originating in the lower atmosphere and extending into the upper atmosphere, is responsible for thermospheric winter polar warming [Bel l et al., 2007]. A major branch of this thesis builds upon the previous work of Muller-Wodarg et al. [2000], Muller-Wodarg et al. [2003], Muller-Wodarg et al. [2006], and Yelle et al. [2006] in order to explain the structures in Titan’s upper atmosphere, between 500 - 1500 km. Building also upon the recent development of GITM by Ridley et al. [2006], this thesis presents a new theoretical framework, T- GITM. This model is then employed to conduct a series of numerical experiments to quantify the impacts of the solar cycle, the season, and the lower boundary winds on Titan’s thermospheric structure and dynamics. Ultimately, these numerical experiments with T-GITM function to validate a newly created Titan upper atmosphere model that has been shown to serve as a viable theoretical and numerical tool for the planetary aeronomy community.