Fig. A.1.
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Initial model we use for the evolution calculations, resulting from planet formation model of Ormel et al. (2021). Metallicity (black) and temperature (red) profiles for a planet formed by rocky pebble accretion at 0.2 AU. The temperature in the classical core region that is not modeled in the formation model, is fitted by isentropic profile in the evolution model. See text for details.
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