Mantle Convection In Super-earths: An Effect Of Adiabatic Compression

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We have studied solid mantle convection in massive terrestrial planets, so-called super-Earths, by using numerical simulation for compressible thermal convection. The mantle convection of terrestrial planets highly affects on their surface environment driving plate tectonics and degassing. On the other hand, the thermal transfer of mantle convection is also very important for core dynamo and magnetic shielding of surface from hazardous stellar wind.
The main differences between mantle convection in both of Earth and super-Earths are gravity acceleration and mantle thickness.
Increase in these quantities results in sufficient adiabatic compression, and it highly affects on the stability of mantle convection.
The magnitude of adiabatic compression is represented by a non-dimensional number, dissipation number that is proportional to gravity acceleration and mantle thickness.
In the case of the Earth, the dissipation number is about 0.5. On the other hand, the dissipation number of super-Earth with 10 Earth mass is about 5. Thus, an order of magnitude larger adiabatic compression can be affected to mantle convection for the case of super Earths.
We have investigated mantle convection with varying the dissipation number that corresponding to planetary mass to show how it affects on style and thermal transfer efficiency of mantle convection. We will show some simulation results and how different the mantle convection of super-Earths is from that in Earth.

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