Physics
Scientific paper
Dec 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufm.p23e..04h&link_type=abstract
American Geophysical Union, Fall Meeting 2005, abstract #P23E-04
Physics
1060 Planetary Geochemistry (5405, 5410, 5704, 5709, 6005, 6008), 5464 Remote Sensing, 5470 Surface Materials And Properties, 6295 Venus
Scientific paper
Venus' surface can be observed remotely on Venus' nightside using several windows in the near-infrared wavelength range. Although Venus is always shrouded in thick clouds, within the window thermal radiation emitted from the planetary surface penetrates through the thick atmosphere and clouds. To obtain the information on the surface, it is necessary to correct the effects of temporal and spatial variability in cloud transmittance by simultaneous observations at neighboring near-infrared windows and radiative transfer modeling, since scattering by clouds cannot be neglected in the Venus near-infrared windows. The intensity of thermal emission is controlled by the emissivity and temperature of the surface. Since the temporal variation in the temperature in the venusian lower atmosphere is expected to be small, the surface temperature will be approximated as the atmospheric temperature at the same elevation, which is calculated as a function of the altitude. Then, we will be able to estimate the surface emissivities at near-infrared wavelengths. If active volcanoes are erupting hot lavas, we will observe excess radiations. Due to strong dependence of the intensity of thermal emission on temperature, a lava lake formed in the crater of an active volcano as small as 1 km2 will be readily detected.
Hashimoto George L.
Roos-Serote Maarten
Sugita Satoshi
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