  We examine the angular momentum loss and associated rotational spin-down for
magnetic hot stars with a line-driven stellar wind and a rotation-aligned
dipole magnetic field. Our analysis here is based on our previous 2-D numerical
MHD simulation study that examines the interplay among wind, field, and
rotation as a function of two dimensionless parameters, W(=Vrot/Vorb) and 'wind
magnetic confinement', $\eta_\ast$ defined below. We compare and contrast the
2-D, time variable angular momentum loss of this dipole model of a hot-star
wind with the classical 1-D steady-state analysis by Weber and Davis (WD), who
used an idealized monopole field to model the angular momentum loss in the
solar wind. Despite the differences, we find that the total angular momentum
loss averaged over both solid angle and time follows closely the general WD
scaling $\dot {J} \sim \dot {M} \Omega R_A^2$. The key distinction is that for
a dipole field Alfv\`en radius $R_A$ is significantly smaller than for the
monopole field WD used in their analyses. This leads to a slower stellar
spin-down for the dipole field with typical spin-down times of order 1 Myr for
several known magnetic massive stars.
