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Massive exoplanets on extremely tight orbits, such as WASP-12 b, induceequilibrium tides in their host stars. Following the orbital motion of theplanet, the tidal fluid flow in the star can be detected with the radialvelocity method. Its signature manifests as the second harmonics of the orbitalfrequency that mimics a non-zero orbital eccentricity. Using the new radialvelocity measurements acquired with the HARPS-N spectrograph at the TelescopioNazionale Galileo and combining them with the literature data, we show that theapparent eccentricity of WASP-12 b's orbit is non-zero at a 5.8 sigma level,and the longitude of periastron of this apparently eccentric orbit is close to270 degrees. This orbital configuration is compatible with a model composed ofa circular orbit and a signature of tides raised in the host star. The radialvelocity amplitude of those tides was found to be consistent with theequilibrium tide approximation. The tidal deformation is predicted to produce aflux modulation with an amplitude of 80 ppm which could be detected usingspace-born facilities.

An apparently eccentric orbit of the exoplanet WASP-12 b as a radial velocity signature of planetary-induced tides in the host star