12/12/2023 0 Comments Ac unity venusThe optical properties of aerosols have been inferred from their wavelength dependence. The extinction values differ according to different wavelengths. Vertical extinction profiles were obtained from data acquired over several wavelengths in the UV and IR domains with SPICAV/SOIR instruments (Wilquet et al. In Takagi and Iwagami ( 2011), the cloud optical thickness, which includes the optical thickness of the haze layer, was estimated from data collected by the previous entry probes, such as the Soviet Venera series the haze optical thickness from 70 to 90 km at 920 nm was found to be 1.0. The haze optical thickness above the clouds in the polar regions was found to be equal to 0.8 at 365 nm but only 0.06 at low latitudes (Kawabata et al. ( 1996) reported that these haze particles have an effective radius of 0.25☐.05 μm and a refractive index of \( 1.435 \pm 0.02 \) in the North Pole region in the South Pole region, these haze particles have an effective radius of 0.29 ± 0.02 μm and a refractive index of \( 1.45 \pm 0.02 \). From PVO Cloud Photopolarimeter observations, Sato et al. The existence of smaller particles within and above the clouds with an effective radius of 0.23 ± 0.04 μm and a refractive index of 1.45 ± 0.04 was suggested from Pioneer Venus Orbiter (PVO) Cloud Photopolarimeter measurements at 550 nm (Kawabata et al. These particles are most likely composed of concentrated sulfuric acid (Esposito 1984), as deduced from refractive index measurements. The mean particle radius (~ 1 μm) within the cloud layer was previously determined from polarimetry observations in the early 1970s (Hansen and Hovenier 1974). 2015) and from SPICAV-IR and UV solar occultations (Luginin et al. The presence of high-altitude hazes/aerosols was also inferred from the analysis of limb profiles observed by the Venus Monitoring Camera (VMC) onboard ESA’s Venus Express (Vex) (Limaye et al. The upper haze layer was observed at altitudes as high as 90 km (Esposito et al. 47 and 70 km surrounded by thinner hazes above and below. The clouds above Venus consist of a main cloud deck located between approx.
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