  Binary systems of compact objects are strong emitters of gravitational waves
whose amplitude depends on the binary orbital parameters as the component mass,
the orbital semi-major axis and eccentricity. Here, in addition to the famous
Hulse-Taylor binary system, we have studied the possibility to detect the
gravitational wave signal emitted by binary systems at the center of our
galaxy. In particular, recent infrared observation of the galactic center have
revealed the existence of a cluster of stars each of which appears to orbit the
central black hole in $SgrA^*$. For the stars labelled as S2 and S14, we have
studied the emitted spectrum of gravitational wave and compare it with the
sensitivity threshold of space-based interferometers like Lisa and Astrod.
Furthermore, following recent observations, we have considered the possibility
that $SgrA^*$ is actually a binary system of massive black holes and calculated
the emission spectrum as a function of the system parameters. The diffraction
pattern of gravitational waves emitted by a binary system by a cluster of stars
has been also analyzed. We remark that this is only a preliminary-theoretical
work than can acquire more interest in view of the next-coming gravitational
wave astronomy era.
