Fig. 4
Evolution of the eccentricity of planet HD 10180b over 250 kyr starting with eb = 0 at t = 0 (present time) for three different models: In red, the numerical integration is purely Newtonian and do not take into account general relativity (GR). In green, GR is taken into account in the integration. In blue, GR is taken into account and the fit is made with the tidal dissipation constraint (32).
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