Effects of topography on the spin-up of a Venus atmospheric model

Details Effects of topography on the spin-up of a Venus atmospheric model Effects of topography on the spin-up of a Venus atmospheric model

Apr 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007jgre..11204s08h&link_type=abstract

Journal of Geophysical Research, Volume 112, Issue E4, CiteID E04S08

Physics

8

Atmospheric Processes: General Circulation (1223), Atmospheric Processes: Planetary Meteorology (5445, 5739), Planetary Sciences: Solid Surface Planets: Atmospheres (0343, 1060), Planetary Sciences: Solid Surface Planets: Meteorology (3346)

Scientific paper

We study how topography affects the spin-up from rest of a model of the atmosphere of Venus. The simulations are performed with the EPIC model using its isentropic, terrain-following hybrid vertical coordinate, and are forced with the Newtonian-cooling profile used to achieve superrotation in a Venus model with no topography by Lee et al. (2005). We are able to reproduce their results with our model, which was developed independently and uses a different vertical coordinate. Both groups use a horizontal resolution of 5°, which is dictated by the need for reasonable computer runtime and is not a claim of numerical convergence. We find that the addition of topography substantially changes both the evolution and end state of the model's spin-up: the magnitude of the superrotation is diminished from 55 ms-1 to 35 ms-1, and it reaches steady state faster, in a few years instead of a few decades. A large, stationary eddy associated with Ishtar Terra forms that has a local horizontal temperature anomaly of order 2 K at the 0.7 bar level; such a feature may be observable in high-resolution infrared images.

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