  In light of recent substantial updates to spectral type estimations and newly
established intrinsic colours, effective temperatures, and bolometric
corrections for pre-main sequence (PMS) stars, we re-address the theory of
accretion-disc regulated stellar angular momentum (AM) evolution. We report on
the compilation of a consistent sample of fully convective stars within two of
the most well-studied and youngest, nearby regions of star formation: the Orion
Nebula Cluster (ONC) and Taurus-Auriga. We calculate the average specific
stellar AM ($j_{\star}$) assuming solid body rotation, using surface rotation
periods gathered from the literature and new estimates of stellar radii and
ages. We use published Spitzer IRAC fluxes to classify our stars as Class II or
Class III and compare their $j_{\star}$ evolution. Our results suggest that
disc dispersal is a rapid process that occurs at a variety of ages. We find a
consistent $j_{\star}$ reduction rate between the Class II and Class III PMS
stars which we interpret as indicating a period of accretion disc-regulated AM
evolution followed by near-constant AM evolution once the disc has dissipated.
Furthermore, assuming our observed spread in stellar ages is real, we find the
removal rate of $j_{\star}$ during the Class II phase is more rapid than
expected by contraction at constant stellar rotation rate. A much more
efficient process of AM removal must exist, most likely in the form of an
accretion-driven stellar wind or other outflow from the star-disc interaction
region or extended disc surface.
