  Sun-like stellar oscillations are excited by turbulent convection and have
been discovered in some 500 main sequence and sub-giant stars and in more than
12,000 red giant stars. When such stars are near gravitational wave sources,
low-order quadrupole acoustic modes are also excited above the experimental
threshold of detectability, and they can be observed, in principle, in the
acoustic spectra of these stars. Such stars form a set of natural detectors to
search for gravitational waves over a large spectral frequency range, from
$10^{-7}$ Hz to $10^{-2}$ Hz. In particular, these stars can probe the
$10^{-6}$ Hz -- $10^{-4}$ Hz spectral window which cannot be probed by current
conventional gravitational wave detectors, such as SKA and eLISA. The PLATO
stellar seismic mission will achieve photospheric velocity amplitude accuracy
of $~ {\rm cm/s}$. For a gravitational wave search, we will need to achieve
accuracies of the order of $10^{-2}{\rm cm/s}$, i.e., at least one generation
beyond PLATO. However, we have found that multi-body stellar systems have the
ideal setup for this type of gravitational wave search. This is the case for
triple stellar systems formed by a compact binary and an oscillating star.
Continuous monitoring of the oscillation spectra of these stars to a distance
of up to a kpc could lead to the discovery of gravitational waves originating
in our galaxy or even elsewhere in the universe. Moreover, unlike experimental
detectors, this observational network of stars will allow us to study the
progression of gravitational waves throughout space.
