  Transition disc systems are young stars that appear to be on the verge of
dispersing their protoplanetary discs. We explore the nature of these systems
by comparing the stellar accretion rates and disc masses of transition discs
and normal T Tauri stars in Taurus and Ophiuchus. After controlling for the
known dependencies of stellar accretion rate and disc mass and on age, stellar
accretion rate on stellar mass, and disc mass on the presence of stellar or
sub-stellar companions, we find that the normal T Tauri stars show a trend of
stellar accretion rate increasing with disc mass. The transition discs tend to
have higher average disc masses than normal T Tauri stars as well as lower
accretion rates than normal T Tauri stars of the same disc mass. These results
are most consistent with the interpretation that the transition discs have
formed objects massive enough to alter the accretion flow, i.e., single or
multiple giant planets. Several Ophiuchus T Tauri stars that are not known
transition disc systems also have very low accretion rates for their disc
masses. We speculate on the possible nature of these sources.
