Infrared properties of haze particles of Venus

Details Infrared properties of haze particles of Venus Infrared properties of haze particles of Venus

Dec 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981icar...48..482m&link_type=abstract

Icarus, vol. 48, Dec. 1981, p. 482-487. Ministry of Education, Science, and Culture

Computer Science

6

Atmospheric Models, Haze, Infrared Radiation, Phase Shift, Radiant Flux Density, Venus Clouds, Absorptivity, Optical Thickness, Particle Size Distribution, Polarized Radiation, Scattering Coefficients, Sulfuric Acid, Venus Atmosphere, Venus, Infrared, Haze, Particles, Wavelengths, Flux, Polarization, Models, Clouds, Optical Properties, Thickness, Calculations, Procedure, Sulfuric Acid, Composition, Absorption, Opacity, Distribution, Size

Scientific paper

The computed variation of the infrared flux and polarization of Venus as a function of phase angle, based upon multiple-scattering calculations for the cloud model of Kawabata el al. (1980) with an internal heat source, precludes the possibility of sulfuric acid as the composition of the haze particles located above the main cloud. Furthermore, calculations reveal that the haze particle should have a large absorption coefficient at these wavelengths, i.e., k (imaginary part of the complex refractive index) not less than 1.3 at a wavelength of 3.4 microns. The optical thickness of the haze layer must be about 0.15 at 3.4 microns.

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