Fig. 12
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Total heavy element mass (core plus envelope) as a function of planetary mass. Simulated planets (see Table 5) are compared to interior models of observed hot Jupiters from Thorngren et al. (2016), marked with the red line. The color coding in this figure shows the dependence on α. The different panels indicate whether evaporation line effects have been taken into account for the simulations (see Table 4).
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