  We report and comment upon the principal results of an investigation into the
evolution of rotating black holes emitting massless scalar radiation via the
Hawking process. It is demonstrated that a Kerr black hole evaporating by the
emission of scalar radiation will evolve towards a state with $a \approx
0.555M$. If the initial specific angular momentum is larger than this value the
hole will spin down to this value; if it is less it will spin up to this value.
The addition of higher spin fields to the picture strongly suggests the final
asymptotic state of a realistic evaporation process will be characterized by an
$a/M = 0$.
