Venus Wind Spin-up Experiments with Topography; Sensitivity to Model Resolution

Details Venus Wind Spin-up Experiments with Topography; Sensitivity to Model Resolution Venus Wind Spin-up Experiments with Topography; Sensitivity to Model Resolution

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufm.p33b1294s&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #P33B-1294

Astronomy and Astrophysics

Astronomy

5405 Atmospheres (0343, 1060), 5445 Meteorology (3346)

Scientific paper

We present new increased-resolution Venus spin-up experiments with topography using the latest hybrid vertical coordinate EPIC atmosphere model (Dowling et. al., Icarus, 182, 2006). We previously reported lower-resolution simulations and showed that the presence of topography substantially accelerates the spin-up of Venusian superrotating winds (Herrnstein and Dowling, JGR, 112, 2007). Our experiments also showed that, with 5- degree resolution, a large stationary eddy develops over Ishtar Terra, north-polar highland region. Here, we test the sensitivity of our previous results to the model resolution, and investigate the effect of finer-scale topographic features on the wind spin-up. Topographic features including an equatorial mountain range were recently discovered on Titan, another slow-rotating planetary body with a thick atmosphere (Stofan et. al., Icarus 186, 2006), and we explore the effects of Titan mountain ranges on the superrotation spin-up also. We aim to compare the effects of prominent topographic features on the resulting equator-to-pole Hadley circulations when the mountains are in the polar region (e.g., Venus) and when they are around the equator (Titan). This research is funded by the NSF Planetary Astronomy Program and NASA Planetary Atmospheres Program.

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