  We present a new model for protoplanetary disc evolution. This model combines
viscous evolution with photoevaporation of the disc, in a manner similar to
Clarke, Gendrin & Sotomayor (2001). However in a companion paper (Alexander,
Clarke & Pringle 2006a) we have shown that at late times such models must
consider the effect of stellar radiation directly incident on the inner disc
edge, and here we model the observational implications of this process. We find
that the entire disc is dispersed on a time-scale of order $10^5$yr after a
disc lifetime of a few Myr, consistent with observations of T Tauri (TT) stars.
We use a simple prescription to model the spectral energy distribution of the
evolving disc, and demonstrate that the model is consistent with observational
data across a wide range of wavelengths. We note also that the model predicts a
short ``inner hole'' phase in the evolution of all TT discs, and make
predictions for future observations at mid-infrared and millimetre wavelengths.
