Fig. A.1
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Comparison between the output of POSIDONIUS and Figure 6 in Bolmont et al. (2017) for the evolution of the semimajor axis of a Jupiter-mass planet, due to the dynamical tide and for different initial stellar rotation periods (1, 3, and 8 days). The dashed curves on this plot correspond to the cyan curves in Figure 6 in Bolmont et al. (2017), which were computed for a solar metallicity (Z = 0.0134).
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