Venus Cloud Structure and Radiative Energy Balance of the Mesosphere
(Sprache: Englisch)
A dense cloud layer located at 5075 km altitude completely covers Venus. The cloud aerosol consists mainly of sulfuric acid mixed with still unknown constituents. Due to their great opacity, the clouds play an important role in the radiative energy balance,...
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A dense cloud layer located at 5075 km altitude completely covers Venus. The cloud aerosol consists mainly of sulfuric acid mixed with still unknown constituents. Due to their great opacity, the clouds play an important role in the radiative energy balance, the general circulation, and the atmospheric chemistry. The knowledge about the upper part of the clouds is especially important to understand the Venus mesosphere, because it is responsible for thermal cooling and solar heating that eventually results in the strongest retrograde zonal wind near the cloud tops in all altitudes. Remote observations have indicated significant temporal and spatial variations of the cloud structure that should affect radiative energy balance of the mesosphere. This thesis investigates the upper cloud layer of Venus. Firstly, the vertical structure of the upper clouds and its variation with latitude are retrieved from the Venus Express observations. For this purpose, we have developed a new technique which uses temperature profiles from the radio science occultation experiment VeRa and thermal emission spectra in the 4.45.0 m range collected by thermal infrared spectrometer VIRTIS. We implemented a comprehensive radiative transfer code including line-by-line calculations of gaseous opacities, and taking account for multiple scattering of aerosols. This study shows significant latitudinal trends in the upper cloud structure. Secondly, we investigated the influence of clouds, and their variability on the thermal fluxes and cooling rates calculated in a broad spectral range (3.86200 m). We developed and used an atmospheric model based on the derived parameters of the upper cloud and the observed temperature field. The result, thermal cooling rates, is compared with the solar heating rates to derive the radiative energy balance.
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The Venus atmosphere can be divided into the upper atmosphere (100 km altitude) and lower atmosphere (100 km) (Schubert et al. 2007), according to the dominant atmospheric circulation. The upper atmosphere is dominated by subsolar-to-antisolar circulation driven by day/night insolation contrast (Lellouch et al. 1997). The lower atmosphere rotates in the zonal retrograde direction. The speed of the strong retrograde flow can reach more than 100 m/s at the cloud tops, and travels the globe in four Earth days, which is 60 times faster than the solid body rotation of the planet. This circulation is the one of the key dynamic features of the lower atmosphere, but its driving mechanism is unknown yet.
Bibliographische Angaben
- Autor: Yeon Joo Lee
- 2012, 1st ed., 150 Seiten, Maße: 15,2 x 21,1 cm, Kartoniert (TB), Englisch
- Verlag: uni-edition
- ISBN-10: 3942171686
- ISBN-13: 9783942171687
- Erscheinungsdatum: 02.08.2012
Sprache:
Englisch
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