Studies of Planetary Atmospheres by Stellar Occultations: Application to Mars and Venus

Abstract

We consider the application of the stellar occultation method to the studies of planetary atmospheres and its history and briefly describe the instruments designed for such measurements (SPICAM/Mars-96, GOMOS/ENVISAT). In comparison with solar occultations, this method allows the profiles to be measured almost at any time of the day and at any location of the planet, irrespective of the orbit of the spacecraft from which observations are carried out. Based on the measuring characteristics of the SPICAM-Light UV spectrometer for the spectral range 118–320 nm with a resolution of 0.9 nm (for the ESA Mars Express Mission; launched in June 2003), we simulate the capabilities of the method to study the Martian atmosphere. In stellar occultation measurements, the stellar spectrum changes because of the absorption by CO2 and O3, other gases, and aerosols. The profiles of the CO2 and O3 density (and, hence, the temperature) and the aerosol content can be restored by solving the inverse problem. Observations of bright stars (no fewer than 30) three to five times in a turn allow us to measure the atmospheric density at altitudes 10–150 km with an accuracy of about 2% and the temperature at altitudes 20–130 km with an accuracy of ≈3 K. Ozone is measured with an accuracy of several percent at altitudes 25–40 km or lower, depending on the conditions. Optically thin clouds and hazes, particularly on the nightside where no measurements are possible in reflected light, can be studied. The SPICAV experiment, which is similar to SPICAM-Light, is part of the Venus Express (to be launched in 2005) scientific payload. On Venus, stellar occultations can be used to measure the atmospheric temperature and density above clouds at altitudes up to 130–150 km and to study the SO2 profile. The results of our simulations can be easily extended to instruments with different measuring characteristics.