Thermal conductivity of MgO in giant planetary interior conditions predicted by deep potential

Abstract

Thermal conductivity $\hat{I}º$ of MgO plays a fundamental role in understanding the thermal evolution and mantle convection in the interior of terrestrial planets. However, previous theoretical calculations deviate from each other and the $\hat{I}º$ of high-pressure B2 phase remains undetermined. Here, by combining molecular dynamics and deep potential trained with first-principles data, we systematically investigate the $\hat{I}º$ of MgO from ambient state to the core-mantle boundary (CMB) of super-Earth with $5M_{\oplus }$. We point out the significance of 4-phonon scatterings and modify the conventional thermal conductivity model of MgO by considering the density-dependent proportion of 3-phonon and 4-phonon scatterings. The $\hat{I}º$ profiles of MgO in Earth and super-Earth are further estimated. For super-Earth, we predict a significant reduction of $\hat{I}º$ at the B1-B2 phase transition area near the CMB. This work provides new insights into thermal transport under extreme conditions and an improved thermal model for terrestrial planets.

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