Physics
Scientific paper
Sep 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000kfnt...16..355m&link_type=abstract
Kinematika i Fizika Nebesnykh Tel, vol. 16, no. 4, p. 355-363
Physics
Scientific paper
The vertical distribution of the haze parameters in the Venusian turbulent atmosphere in simulated on the assumption that the haze above clouds (at heights greater than 66 km) is an extension of mode 1 of the main cloud layer. The ratio between the specific weight of haze particles and the turbulent mixing coefficient, γ/Dt, is found to range from 0.545\cdot10-5 to 1.09\cdot10-5 g\cdot cm-5s. The parameters of the size distribution of haze particles are stratified in height: at γ/Dt = 0.545\cdot10-5g\cdot cm-5s the parameter r0 decreases from 0.175 to 0.043 μm when the height changes from 66 km to 98 km, and the particle size variance σ2 changes from 0.59 to 0.11. This accounts for the difference in the particle size determined from polarization phase curves light and dark features on the planet's disk and from 4-day variations in the polarization of the planet's disk. We also conclude that it is precisely the atmospheric layers with heights greater than 70 km which are responsible for short-period changes in the degree of polarization of the Venusian disk.
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