Wavelength dependence of polarization on Venus. XXXV. Vertical structure of scattering layers above the visible Venus clouds.
Abstract
Results of multiple-scattering computations based on whole-disk and Digicon polarization observations are presented which indicate vertical inhomogeneity in the upper atmosphere of Venus. It is shown that the whole-disk observations support a thin upper haze layer of 0.18-micron particles and that the low polarization observed near the limb and terminator requires a haze of slightly larger particles. The Digicon polar regions are found to exhibit increased polarization, which is compatible with CO2 absorption measurements and is explained by increased molecular scattering above the clouds. The decrease in cloud-top height for latitudes greater than 45 deg is estimated to be approximately 1.4 km.
- Publication:
-
The Astronomical Journal
- Pub Date:
- May 1979
- DOI:
- 10.1086/112468
- Bibcode:
- 1979AJ.....84..683L
- Keywords:
-
- Atmospheric Scattering;
- Frequency Response;
- Polarization (Waves);
- Venus Clouds;
- Vertical Distribution;
- Wavelengths;
- Astronomical Models;
- Atmospheric Models;
- Atmospheric Stratification;
- Graphs (Charts);
- Radiative Transfer;
- Upper Atmosphere;
- Venus Atmosphere;
- WAVELENGTHS;
- POLARIZATION;
- VENUS;
- CLOUD LAYERS;
- SCATTERING;
- CLOUDS;
- MODELS;
- PRESSURE;
- AEROSOLS;
- OBSERVATIONS;
- PHASE ANGLES;
- ATMOSPHERE;
- LIMBS;
- TERMINATORS;
- THICKNESS;
- GRAIN SIZE;
- ULTRAVIOLET;
- Lunar and Planetary Exploration; Venus;
- Albedo:Venus Atmosphere;
- Polarization:Venus Atmosphere;
- Venus Atmosphere:Clouds