  To date, asteroseismology has provided core to surface differential rotation
measurements in eight main-sequence stars. These stars, ranging in mass from
$\sim$1.5-9$M_\odot$, show rotation profiles ranging from uniform to
counter-rotation. Although they have a variety of masses, these stars all have
convective cores and overlying radiative regions, conducive to angular momentum
transport by internal gravity waves (IGW). Using two-dimensional (2D) numerical
simulations we show that angular momentum transport by IGW can explain all of
these rotation profiles. We further predict that should high mass, faster
rotating stars be observed, the core to envelope differential rotation will be
positive, but less than one.
