  Close-in, massive exoplanets raise significant tides in their stellar hosts.
We compute the radial velocity (RV) signal due to this fluid motion in the
equilibrium tide approximation. The predicted radial velocities in the observed
sample of exoplanets exceed 1 m/s for 17 systems, with the largest predicted
signal being ~30 m/s for WASP-18 b. Tidally-induced RV's are thus detectable
with present methods. Both tidal fluid flow and the epicyclic motion of a
slightly eccentric orbit produce an RV signal at twice the orbital frequency.
If care is not taken, the tidally induced RV may, in some cases, be confused
with a finite orbital eccentricity. Indeed, WASP-18 b is reported to have an
eccentric orbit with small e=0.009 and pericenter longitude \omega=-\pi/2.
Whereas such a close alignment of the orbit and line of sight to the observer
requires fine tuning, this phase in the RV signal is naturally explained by the
tidal velocity signature of an e=0 orbit. Additionally, the equilibrium tide
estimate for the amplitude is in rough agreement with the data. Thus the
reported eccentricity for WASP-18 b is instead likely a signature of the
tidally-induced RV in the stellar host. Measurement of both the orbital and
tidal velocity for non-transiting planets may allow planet mass and inclination
to be separately determined solely from radial velocity data. We suggest that
high precision fitting of RV data should include the tidal velocity signal in
those cases where it may affect the determination of orbital parameters.
