Abstract
Most of our knowledge regarding planetary atmospheric composition and structure has been achieved by remote sensing spectroscopy. Planetary spectra strongly differ from one planet to another. CO2 signatures dominate on Mars, and even more on Venus (where the thermal component is detectable down to 1 μm on the dark side). Spectroscopic monitoring of Venus, Earth and Mars allows us to map temperature fields, wind fields, clouds, aerosols, surface mineralogy (in the case of the Earth and Mars), and to study the planets’ seasonal cycles. Spectra of giant planets are dominated by H2, CH4 and other hydrocarbons, NH3, PH3 and traces of other minor compounds like CO, H2O and CO2. Measurements of the atmospheric composition of giant planets have been used to constrain their formation scenario.
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