  We present the results of a spectroscopic investigation of 108 nearby field
B-stars. We derive their key stellar parameters, $V \sin i$, $T_{\rm eff}$,
$\log g$, and $\log g_{\rm polar}$, using the same methods that we used in our
previous cluster B-star survey. By comparing the results of the field and the
cluster samples, we find that the main reason for the overall slower rotation
of the field sample is that it contains a larger fraction of older stars than
found in the (mainly young) cluster sample.
