Fig. 10
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Mass-radius diagrams for the small planet sample with measured dynamical masses with a precision better than 20%. Left: color coding indicates the stellar host metallici ties. TOI-244 b is not filled with any color since we get inconsistent metallicities with the different methods used (see Sect. 3.2). The dashed and dotted lines correspond to theoretical interior models that consider different mass percentages of Fe and MgSiO3 (Zeng et al. 2016, Zeng et al. 2019). Right: color coding indicates the stellar insolation received by the planets. The dashed lines correspond to theoretical models from Zeng et al. (2019), which consider planets without a significant amount of volatiles (back and red lines), planets with condensed water (dark blue), and planets with H2 atmospheric envelopes (light blue). The dotted lines correspond to the Turbet et al. (2020) theoretical models for Earth-like planets with H2O-dominated atmospheres. These plots have been prepared using mr-plotter, which is available at https://github.com/castro-gzlz/mr-plotter/.
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