  We present a description for the angular momentum loss rate due to magnetic
braking for late type stars taking into account recent observational data on
the relationship between stellar activity and rotation. The analysis is based
on an idealized two component coronal model subject to constraints imposed on
the variation of the coronal gas density with rotation period inferred from the
observed variation of X-ray luminosity, L_x, with rotation rate, Omega, (L_x
\propto Omega^2) for single rotating dwarfs. An application of the model to
high rotation rates leads to a gradual turnover of the X-ray luminosity which
is similar to the saturation recently observed in rapidly rotating dwarfs. The
resulting angular momentum loss rate, \dot J, depends on Omega in the form \dot
J \propto Omega^beta where beta ~ 3 for slow rotators and ~ 1.3 for fast
rotators. The relation at high rotation rates significantly differs from the
power law exponent for slowly rotating stars, depressing the angular momentum
loss rate without necessarily requiring the saturation of the magnetic field.
The application of this model to the evolution of cataclysmic variable binary
systems leads to mass transfer rates that are in approximate accord with those
observed in comparison to rates based on either a Skumanich law or an empirical
law based on beta=1.
