Venus Cloud Particle Properties Using VIRTIS / Venus Express Data.

Details Venus Cloud Particle Properties Using VIRTIS / Venus Express Data. Venus Cloud Particle Properties Using VIRTIS / Venus Express Data.

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007dps....39.5802g&link_type=abstract

American Astronomical Society, DPS meeting #39, #58.02; Bulletin of the American Astronomical Society, Vol. 39, p.533

Statistics

Methodology

Scientific paper

We present an analysis of infrared emission from the nightside of Venus, taken using the VIRTIS instrument. This radiation, coming from the deep atmosphere, is scattered and absorbed by clouds and atmospheric compounds, before escaping through some narrow spectral windows. As the optical properties of cloud particles depend on both their sizes and wavelength of incoming radiation, we analyse the correlation of radiance emitted at two different wavelengths in an attempt to deduce information about particle sizes.
Following the methodology of Carlson et al. [1993], we realized correlation plots of the radiance at 1.7 microns as a function of the radiance at 2.3 microns : different branches are seen, indicative of clouds comprised of different particle sizes. At first, a 'size parameter', defined as m = ( I2.30um ) 0.53 / ( I1.74um ), is used to characterize these branches. We found that this parameter shows a marked increase polewards of 70 degrees latitude, in both the Southern and Northern hemispheres, indicating larger cloud particles in the polar regions. Spatial variations elsewhere on the planet are relatively small.
We present radiative transfer modeling to support our data interpretation. Sensitivity to changes in the height of the clouds has been studied. However, as the number of parameters is high, we chose to specify the altitude, composition and size distribution of the four particle modes derived from descent probes measurements. For cloud models that comprise of several modes of particles, the problem being under-constrained, the model generates non-unique solutions. This modeling work highlighted some problems with the use of the simplistic 'size parameter'. We also consider the contribution of changes in atmospheric temperature to variations observed in the 1.7/2.3 um ratio; and consider information available from other near-IR windows, particularly at 1.31 um.

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