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FN CMa is visually double with a separation of about 0.6arcsec. Sixtyhigh-cadence VLT/UVES spectra permit the A and B components to be disentangled,as the relative contribution of each star to the total light entering thespectrograph fluctuates between exposures due to changes in seeing. Component Aexhibits rapid line-profile variations, leading us to attribute the photometricvariability seen by HIPPARCOS (with a derived P=0.08866d) to this component.From a total of 122 archival and new echelle spectra it is shown that componentA is an SB1 binary with an orbital period of 117.55 days. The eccentricity of0.6 may result in tidal modulation of the pulsation(s) of component Aa.

The (B0+?)+O6 system FN CMa: A case for tidal-pulsational interaction?