  Experimental evidences indicate that formations of disks and planetary
systems around pulsars are allowed. Unfortunately, direct detections through
electromagnetic observations appear to be quite rare. In the case of PSR
1931+24, the hypothesis of a rigid precessing disk penetrating the pulsar light
cylinder is found consistent with radio transient observations from this star.
Disk self-occultation and precession may limit electromagnetic observations.
Conversely, we show here that gravitational waves generated by disk precessing
near the light cylinder of young and middle aged pulsars would be detected by
future space interferometers with sensitivities like those expected for DECIGO
(DECI-hertz Interferometer Gravitational Wave Observatory) and BBO (Big Bang
Observer). The characteristics of circumpulsar detectable precessing disks are
estimated as a function of distance from the Solar System. Speculations on
upper limits to detection rates are presented.
