  We present evidence of magnetically-mediated disk accretion in Herbig Ae/Be
stars. Magnetospheric accretion models of Balmer and sodium profiles calculated
with appropriate stellar and rotational parameters are in qualitative agreement
with the observed profiles of the Herbig Ae star UX Ori, and yield a mass
accretion rate of ~ 10^{-8} Msun/yr. If more recent indications of an extremely
large rotation rate for this object are correct, the magnetic field geometry
must deviate from that of a standard dipole in order to produce line emission
consistent with observed flux levels. Models of the associated accretion shock
qualitatively explain the observed distribution of excess fluxes in the Balmer
discontinuity for a large ensemble of Herbig Ae/Be stars, and imply typically
small mass accretion rates, < 10^{-7} Msun/yr. In order for accretion to
proceed onto the star, significant amounts of gas must exist inside the dust
destruction radius, which is potentially problematic for recently advocated
scenarios of "puffed" inner dust wall geometries. However, our models of the
inner gas disk show that for the typical accretion rates we have derived, the
gas should be generally optically thin, thus allowing direct stellar
irradiation of the inner dust edge of the disk.
