Physical properties of MgO at deep planetary conditions

Abstract

Using ab initio molecular dynamics simulations, we calculate the physical properties of MgO at conditions extending from the ones encountered in the Earth mantle up to the ones anticipated in giant planet interiors such as Jupiter. We pay particular attention to the high pressure melting temperature throughout this large density range as this is a key ingredient for building accurate planetary interior models with a realistic description of the inner core. We compare our simulation results with previous ab initio calculations that have been so far limited to the pressure range corresponding to the Earth mantle and the stability of B1-B2 transition around 6 Mbar. We provide our results for both the EOS and high pressure melting curve in parametric forms for direct use in planetary models. Finally, we compare our predictions of the high pressure melting temperature with various interior profiles to deduce the state of differentiated layer within the core made of MgO in various types of planets and exoplanets.

arXiv comment7 figures

References in corpus (9)

• Detailed Models of super-Earths: How well can we infer bulk properties?
• Generation of Projector Augmented-Wave atomic data: a 71 elements validated table in the XML format
• Radius and Structure models for the First Super-Earth Planet
• Jupiter models with improved ab initio hydrogen EOS (H-REOS.2)
• The melting curve of MgO from first principles simulations
• Shock Response and Phase Transitions of MgO at Planetary Impact Conditions
• Jupiter internal structure: the effect of different equations of state
• Decaying shock studies of phase transitions in MgOSiO2 systems: implications for the Super-Earths interiors
• The melting curve of iron at extreme pressures: implications for planetary cores

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