Upcoming space-based photometric satellites offer the possibility of detecting continuum flux variability at the micromagnitude (μmag) level. We show that the Doppler flux variability induced by the reflex motion of stars due to planetary companions has an amplitude of (3-α)K/c, where K is the reflex radial velocity amplitude and α~(dlnFν/dlnν) is the logarithmic slope of the source spectral flux in the observed frequency band. For many of the known close-in planetary systems with periods P<~0.2 yr, the periodic Doppler variability, O(μmag), is significant relative to the variability caused by reflected light from the planetary companion. For companions with P>~0.2 yr, the Doppler signal is larger than the reflected light signal. We show that the future photometric satellites should reach the sensitivity to detect this Doppler variability. In particular, the Kepler satellite should have the photon noise sensitivity to detect at a signal-to-noise ratio >~5 all planets with minimum mass Mpsini>~5MJ and P<~0.1 yr around the ~104 main-sequence stars with spectral types A-K and apparent magnitude V<12 in its field of view.
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