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The code is parallelized; with 12 processors the speedup factor is about 9. The solutions of model core convection with and without rotation are discussed.
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As these gyres are concentrated at low latitudes, core convection expels them and pushes them westward, the model shows.
According to these models, a few tens of Myrs after inner core nucleation outer core convection indeed becomes dominantly chemical.
In conclusion, whether a terrestrial planet features core convection and whether it can have a thermal or a chemical dynamo in these models depends mainly on the cooling rate of the core, the core temperatures, and the core melting temperatures.
Core convection produces Earth's magnetic field, which may influence surface conditions, and mantle convection causes volcanism, seafloor generation, and mountain building.
The CHORUS code creates new opportunities for simulating such varied phenomena as multi-scale solar convection, core convection, and convection in rapidly-rotating, oblate stars.
A semi-implicit multi-layer spherical spectral method for simulating stellar core convection is described.
Without that flow, core convection grinds to a halt.
A massive collision could warm Mars's mantle, disrupting core convection.
This may provide a glimpse into the history of core convection.
The extra heat was enough to stop core convection, the team reports in the current issue of the Journal of Geophysical Research – Planets.
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