Fig. 5
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Temperature profiles of a selected set of planet masses and Ṁpeb = 10−7 M⊕ yr−1. Colors and line styles have the same meaning as in Fig. 2. At a given mass, the envelopes are slightly colder than in the nominal case Ṁpeb = 10−6 M⊕ yr−1. As a result, the enriched envelopes start to differ from the pure H2/He envelopes only after Mpl > 0.4 M⊕.
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