  We examine He I 10830 profile morphologies for a sample of 56 Herbig Ae/Be
stars (HAEBES). We find significant differences between HAEBES and CTTSs in the
statistics of both blue-shifted absorption (i.e. mass outflows) and red-shifted
absorption features (i.e. mass infall or accretion). Our results suggest that,
in general, Herbig Be (HBe) stars do not accrete material from their inner
disks in the same manner as CTTSs, which are believed to accrete material via
magnetospheric accretion, while Herbig Ae (HAe) stars generally show evidence
for magnetospheric accretion. We find no evidence in our sample of narrow
blue--shifted absorption features which are typical indicators of inner disk
winds and are common in He I 10830 profiles of CTTSs. The lack of inner disk
wind signatures in HAEBES, combined with the paucity of detected magnetic
fields on these objects, suggests that accretion through large magnetospheres
which truncate the disk several stellar radii above the surface is not as
common for HAe and late-type HBe stars as it is for CTTSs. Instead, evidence is
found for smaller magnetospheres in the maximum red-shifted absorption
velocities in our HAEBE sample. These velocities are, on average, a smaller
fraction of the system escape velocity than is found for CTTSs, suggesting
accretion is taking place closer to the star. Smaller magnetospheres, and
evidence for boundary layer accretion in HBe stars, may explain the less common
occurrence of red--shifted absorption in HAEBES. Evidence is found that smaller
magnetospheres may be less efficient at driving outflows compared to CTTS
magnetospheres.
