  Cool main-sequence, sub-giant and red-giant stars all show solar-like
oscillations, pulsations that are excited and intrinsically damped by
near-surface convection. Many overtones are typically excited to observable
amplitudes, giving a rich spectrum of detectable modes. These modes provide a
wealth of information on fundamental stellar properties. However, the radial
velocity shifts induced by these oscillations can also be problematic when
searching for low-mass, long-period planets; this is because their amplitudes
are large enough to completely mask such minute planetary signals. Here we show
how fine-tuning exposure times to the stellar parameters can help efficiently
average out the solar-like-oscillation-induced shifts. To reduce the
oscillation signal to the radial velocity precision commensurate with an
Earth-analogue, we find that for cool, low-mass stars (near spectral type K)
the necessary exposure times may be as short as 4 minutes, while for hotter,
higher-mass stars (near spectral type F, or slightly evolved) the required
exposure times can be longer than 100 minutes. We provide guideline exposure
durations required to suppress the total observed amplitude due to oscillations
to a level of $0.1\,\rm m\,s^{-1}$, and a level corresponding to the
Earth-analogue reflex amplitude for the star. Owing to the intrinsic stochastic
variability of the oscillations, we recommend in practice choosing short
exposure durations at the telescope and then averaging over those exposures
later, as guided by our predictions. To summarize, as we enter an era of
$0.1\,\rm m\,s^{-1}$ instrumental precision, it is critical to tailor our
observing strategies to the stellar properties.
