CESM was used to perform aquaplanet and drycore simulations. Heat anomalies were injected into the SSTs of aquaplanets and surface anomalies were used for drycore simulations. Anomalies were constructed using different geometries such as disk and bands with constant latitudes. The goal is to explore the effect of these heat anomalies on the polar vortex.
Aquaplanet
Below are figures for a disk SST anomaly at 30N. The field shown is the geopotential height at 250 hPa. Also shown is the power spectra for the same field.
Below are figures for a band SST anomaly at 30N. The field shown is the geopotential height at 250 hPa. Also shown is the power spectra for the same field.
Drycore
Below are figures for a disk surface anomaly at 30N. The field shown is the geopotential height at 250 hPa. Also shown is the power spectra for the same field.
Below are figures for a band surface anomaly at 30N. The field shown is the geopotential height at 250 hPa. Also shown is the power spectra for the same field.
Drycore with Lapse Rate
Below are figures for a disk surface anomaly at 30N. A vertical lapse rate was included in these simluations. The field shown is the geopotential height at 250 hPa. Also shown is the power spectra for the same field.
Below are figures for a band surface anomaly at 30N. A vertical lapse rate was included in these simluations. The field shown is the geopotential height at 250 hPa. Also shown is the power spectra for the same field.
More figures shown in the following slideshow.
