Fig. 10

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Resulting best-fit model as function of the mass of the white dwarf. The inclination, i, of the system (top), the resulting K half velocityamplitude (middle), and the orbital separation of the mass centers of the stars (bottom panel). The dashed line marks the average between the extreme cases of the emission and the absorption line velocities, while the dotted lines mark the two extreme cases (see text).
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