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Fig. 6


Forced eccentricity ef, as a function of the semimajor axes of the binary aB and the planetesimal a, for all the orbital solutions of γ-Cephei with residuals within the 1σ confidence level of the best fit. Top and bottom frames assume two different values for mA. Each value of aB implies different values of both mB and eB, obtained from the families of orbital fits presented in Fig. 5. Values of aB for each best fit are shown with horizontal dashed lines.

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