A model for Hot Jupiter with bottom thermal perturbation
Abstract
Hot Jupiters are one of the few types of planets that can currently be observationally characterized. Under strong external radiation forcing, Hot Jupiters show a variety of atmosphere circulation pattern. Due to spectrum exhibits information and our knowledge in atmosphere dynamic of the Hot Jupiter, some researchers create the atmosphere models, for understanding the observations and the physics of these planets generally, but almost all models ignore — or treat in a very simplified fashion — the interaction of the interior convection zone with the deep, thick stratified atmosphere. Here, we take the small-scale thermal perturbation into account, and import a spatially and temporally noise, which is horizonally isotropic, as forcing parameter into 3D primitive equation model for influencing the temperature at convective-radiation boundary layer. In some cases, the random thermal perturbation give limited impact on pattern — a significant temperature increase near the hot spot, while the others does not have much influence on the top layer pattern, which shows hot spot shift with super-rotation on equator at top layers, when star radiation becomes stronger.We draw a conclusion that the flow does not vary in time until the bottom perturbation is over the bottom heating rate(0.001K/sec). We assume the model relax the radiation forcing by Newtonian cooling scheme to equivalent temperature in various radiative time scale on different levels.Perhaps we predict more time variability if atmospheres are strongly enough forced by convection, and we hope get new information from spectrum to prove the result.
- Publication:
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AAS/Division for Extreme Solar Systems Abstracts
- Pub Date:
- August 2019
- Bibcode:
- 2019ESS.....431303L