The low-energy charged particle (LECP) experiment observed satellite microsignatures in ions (28 keV-4 MeV) and electrons (22keV--20 MeV) during the Voyager encounters with Saturn in 1980 and 1981. Each of the five major satellites within the orbit of Titan had associated with it at least one absorption feature in the high time resolution (400 ms) data. Generally, microsignatures involve abrupt rate decreases of factors up to 10 or more, lasting on time scales less than 2 min. Occasionally, substructure within the microsignature is observed on time scales of 5--10 s at a single pitch angle. Pitch angle distributions and spectral behavior of low-energy ions (28--500 keV) imply that particles of low energy with pitch angles near 90¿ are absorbed most efficiently. Microsignatures are usually observed in the corotational wake region within ~25¿ in azimuth of a satellite. The peculiar microsignature observed in the vicinity of Enceladus may suggest clumping of E ring material similar to clumping known to exist in the F ring. A microsignature in both ions and electrons (~450 km wide) observed at the expected crossing of Mimas' L shell outbound exhibits characteristics that are not fully consistent with it being due to Mimas. The microsignature could be interpreted as due to material co-orbiting with Mimas ~147¿ ahead of the satellite. We use the microsignature of Dione to deduce the diffusion coefficient of ~25 to ~100 keV electrons and find D≂10-7 RS2/s at L≂6.3 i.e., much faster (~103) than diffusion rates estimated at the orbit of Mimas (L≂3) for MeV electrons (Van Allen et al., 1980c). Microsignatures do not generally occur at times predicted by a centered, aligned dipole; a better predictive model seems to be that of an aligned, axisymmetric field with significant quadrupole and octupole terms.