Studying the Structure and Composition of the Atmosphere of Mars by High-Resolution Infrared Heterodyne Spectroscopy

点击翻译按钮获取中文摘要

Understanding of the physical processes in planetary atmospheres is essential for the development of general circulation models (GCM) and for longterm climate predictions. Besides the Earth, this is of high interest especially for the terrestrial planets Mars and Venus. Simulation of a number of key parameters in the used models like wind velocity, temperature, molecular abundances or pressure leads to a detailed prediction of the atmospheric behaviour including atmospheric chemistry. An ideal tool for remote sensing of planetary atmospheres is high spectral resolution infrared heterodyne spectroscopy. In contrast to microwave observations an adequate spatial resolution can be achieved easily in addition to the high spectral resolution. From fully resolved molecular lines velocity, temperature or abundance of the emitting and absorbing gas can be directly deduced. Especially in the case of Mars, atmospheric models have improved substantially over the last years due to data from several space missions. Nevertheless these data are selective and from limited altitude regions of Mars. Additional observations from other (mostly higher) atmospheric regions are necessary to constrain and validate models and support the interpretation of lower resolution data. Heterodyne measurements can provide complimentary information like upper atmosphere winds or vertical gas abundance profiles thus leading to an improved understanding of the Martian atmosphere including, on the side, a look at Mars as an exo-planet prototype. The proposed work will also include efforts in education and public outreach specifically aimed at children.