Long-term (up to 10 000 d) monitoring has been undertaken for 41 Seyferts in the near-infrared (1.25–3.45 μm). All but two showed variability, with amplitudes at K in the range <0.1 to >1.1 mag. The time-scale for detectable change is from about one week to a few years. Where contemporary observations of variability in X-rays, ultraviolet (UV) or visible light exist, it is found that the near-infrared varies in a similar way, though in some cases the shorter-wavelength infrared (IR) bands are diluted by underlying galaxy radiation. A simple cross-correlation study indicates that there is evidence for delays of up to several hundred d between the variations seen at the shortest wavelengths (U or J) and the longest (L) in many galaxies. In particular, the data for Fairall 9 now extend to twice the interval covered in earlier publications and the delay between its UV and IR outputs is seen to persist. An analysis of the fluxes shows that, for any given galaxy, the colours of the variable component of its nucleus are usually independent of the level of activity. The state of activity of the galaxy can be parameterized. Taken over the whole sample, the colours of the variable components fall within moderately narrow ranges. In particular, the H−K colour is appropriate to a blackbody of temperature 1600 K. The H−K excess for a heavily reddened nucleus can be determined and used to find EB−V, which can be compared to the values found from the visible region broad line ratios. Using flux–flux diagrams, the flux within the aperture from the underlying galaxies can often be determined without the need for model surface brightness profiles. In many galaxies it is apparent that there must be an additional constant contribution from warm dust.