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Fig. 7


Constraints on the third body in the K2-111 system. Solid lines show the minimum masses required to reproduce the RV trend, as a function of the third body’s orbital period and eccentricity. Dotted lines show the maximum masses allowed for dynamical stability for these periods and eccentricities (Gladman 1993; Petrovich 2015). The dashed black line shows the final masses of planets produced in the planet formation model of Bitsch et al. (2015) with a metallicity [ Fe / H ] = − 0.5. This model successfully forms super-Earths which migrate to K2-111 b’s location at the inner disc edge, and predicts that the second body would have a mass of 20–50 M. K2-111 b.

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