The figure shows the signals that would be generated by a compact object of mass 5 M☉ inspiralling into a massive black hole. The orbit used in the calculation is circular with radius r = 7 GM/c2, inclined at 62o to the equatorial plane of the massive black hole. The observer is assumed to be at a distance of 1 Gpc in the equatorial plane of the massive black hole.
The gravitational waveforms occur in two polarizations: + (blue line) and x (red line). The low-frequency amplitude modulation of the waveforms is due to Lense-Thirring precession, i.e. the dragging of the orbit's nodes by the black hole's spin. The compact object is losing angular momentum and energy to infinity through gravitational radiation, but is gaining back a small but measurable fraction of those losses due to superradiant scattering of the gravitational waves it sends into the black hole's ergosphere.
For clarity, only 1.5 days of waveform are shown, but LISA would be able to observe such waveforms for the years it would take the compact object to spiral into the massive black hole, mapping the details of Kerr geometry as it goes.
The axes can be scaled to other circumstances: the time unit on the abscissa is proportional to the mass of the central black hole, and the wave amplitude on the ordinate to the mass of the inspiralling compact object divided by the distance between the source and the Sun