Temperature and Density on the Forsterite Liquid‐Vapor Phase Boundary

Abstract

During terrestrial planet formation, impacts were a widespread and fundamental process (Chambers, 2010), the scale of which ranged from small impacts between planetesimals to giant impacts such as the Moon-forming impact. The post-impact structures of a giant impact depend upon the specific parameters of the impact. The equations of state (EOS) of the constituent materials are necessary to enable calculation of the energy deposited by the event and the internal structure, including the amount of melting and vaporization. Previous work has found that energetic, high-angular momentum impacts create synestias (Lock & Stewart, 2017;Lock et al., 2018) and less energetic impacts form a more traditional planet and disk structures (Canup et al., 2013). Understanding the evolution of planetary bodies after a giant impact requires robust EOS models.

Modeling of shock-wave loading of magnesium silicates on the example of forsterite

“…Magnesium silicates and their high pressure phases are major components of the Earth and possibly of other inner planets of the Earth group. In this regard, forsterite, for which there are experimental data on high-energy effects, can be used in simulation of planetary collisions, which are an important process in the formation and evolution of planets [1]. A detailed understanding of both the physical and chemical processes that occur during and just after the collision of astronomical bodies motivates an accurate description of forsterite at pressures and temperatures significantly exceeding those corresponding to the interior of the Earth [2].…”