Infrared polarization of Venus - Its periodic fluctuations and evidence for thin haze

Details Infrared polarization of Venus - Its periodic fluctuations and evidence for thin haze Infrared polarization of Venus - Its periodic fluctuations and evidence for thin haze

Jan 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984icar...57..125n&link_type=abstract

Icarus (ISSN 0019-1035), vol. 57, Jan. 1984, p. 125-134.

Astronomy and Astrophysics

Astronomy

6

Haze, Infrared Astronomy, Optical Polarization, Optical Thickness, Periodic Variations, Venus Atmosphere, Brightness Temperature, Microparticles, Phase Shift, Thermal Emission, Venus Clouds, Venus, Infrared, Wavelengths, Polarization, Atmosphere, Haze, Thickness, Polarimetry, Thermal Effects, Emissions, Polar Regions, Fluctuations, Equatorial Regions, Comparisons, Models, Calculations, Optical Properties, Clouds, Haze, Layers, Brightness, Temperature

Scientific paper

The Sato et al. (1980) IR polarimetry measurements of Venus have been extended to cover the phase angles from 18 to 171 deg. For the case of 2.25-5.0 micron polarization measurements, a remarkable variation with wavelength is found in the 2.2-4.2 micron filter region, together with a decrease with increasing field-of-view at 5.0 microns due to the contamination of thermal emission from the dark crescent. Comparisons with model calculations indicate that these results confirm the existence of a thin haze layer which consists of submicron-size particles above the main clouds of Venus. The 4.5-5.0 day fluctuations found could be due to a variation of the optical thickness of the haze layer, or of the brightness temperature of the main clouds.

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