Planetary-scale waves in the Venus atmosphere.
Abstract
Observed wave-like cloud features on Venus, which at times form a Y-like structure which encircles the planet, were modelled numerically. Linearized primitive equations for a shallow, hydrostatic atmosphere are defined, along with upper boundary layer conditions for the 4-6 day periods detected in the atmospheric response to forcing. The basic state of the Venus atmosphere was considered to display variations in static stability and the mean zonal wind as a function of altitude. Forcing was introduced over a wide range of frequencies in order to produce the target oscillation modes. Combination of a midlatitude Rossby wave and an equatorial Kelvin wave was found to yield the observed Y-shape, which could be preserved with nonlinear coupling.
- Publication:
-
Journal of the Atmospheric Sciences
- Pub Date:
- November 1982
- DOI:
- 10.1175/1520-0469(1982)039<2397:PSWITV>2.0.CO;2
- Bibcode:
- 1982JAtS...39.2397C
- Keywords:
-
- Atmospheric Models;
- Planetary Waves;
- Venus Atmosphere;
- Atmospheric Circulation;
- Linear Equations;
- Mathematical Models;
- Traveling Waves;
- Wave Propagation;
- Venus Atmosphere:Models