  The spin-down of Be stars due to angular momentum transport from star to disc
has been considered. This has been prompted by empirical studies of observed
optical and IR line profile studies indicating that the disc is rotating in a
Keplerian fashion. It is found that substantial spin-down may occur, especially
for late B stars throughout their main-sequence lives for the ``strongest''
discs (most dense $\sim 10^{-11}$g cm$^{-3}$ with high radial velocity $\sim
1\kms$ at their inner edge and with large opening angle $\sim 15^\circ$). This
is in conflict with studies of rotational velocity distributions for different
luminosity classes, which show no significant evolution. The implications of
this for Be star discs are considered.
