  We use Doppler imaging techniques to determine the dependence of starspot
rotation rates on latitude in an homogeneous sample of young, rapidly-rotating
solar analogues. A solar-like differential rotation law is used, where the
rotation depends on sin$^2$($\theta$), where $\theta$ is the stellar latitude.
By including this term in the image reconstruction process, using starspots as
tracers, we are able to determine the magnitude of the shear over more than one
rotation cycle. We also consider results from matched filter starspot tracking
techniques, where individual starspot rotation rates are determined. In
addition we have re-analysed published results and present a new measurement
for the K3 dwarf, Speedy Mic.
  A total of 10 stars of spectral type G2 - M2 are considered. We find a trend
towards decreasing surface differential rotation with decreasing effective
temperature. The implied approach to solid body rotation with increasing
relative convection zone depth implies that the dynamo mechanism operating in
low-mass stars may be substantially different from that in the Sun.
