Fig. 3.
Comparison between the high-pressure melting temperatures we obtained and density-temperature profiles for the planets of the solar system (red lines). The dashed regions correspond to P–T conditions where the constituent is in a solid state. The adiabats for Saturn, Neptune, and Uranus are from Guillot & Gautier (2014). For Jupiter, we show the adiabats obtained by Nettelmann et al. (2012; dashes) and Militzer & Hubbard (2013; solid).
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