  Detecting binary stars in photometric time series is traditionally done by
measuring eclipses. This requires the orbital plane to be aligned with the
observer. A new method without that requirement uses stellar oscillations to
measure delays in the light arrival time and has been successfully applied to
$\delta$ Scuti stars. However, application to other types of stars has not been
explored. To investigate this we simulated light curves with a range of input
parameters. We find a correlation between the signal-to-noise of the pulsation
modes and the time delay required to detect binary motion. The detectability of
the binarity in the simulations and in real $Kepler$ data shows strong
agreement, hence, we describe the factors that have prevented this method from
discovering binary companions to stars belonging to various classes of
pulsating stars.
