  Recent observational work has indicated that mechanisms for accretion and
outflow in Herbig Ae/Be star-disk systems may differ from magnetospheric
accretion (MA) as it is thought to occur in T Tauri star-disk systems. In this
work, we assess the temporal evolution of spectral lines probing accretion and
mass loss in Herbig Ae/Be systems and test for consistency with the MA
paradigm. For two Herbig Ae/Be stars, HD 98922 (B9e) and V1295 Aql (A2e), we
have gathered multi-epoch (~years) and high-cadence (~minutes) high-resolution
optical spectra to probe a wide range of kinematic processes. Employing a line
equivalent width evolution correlation metric introduced here, we identify
species co-evolving (indicative of common line origin) via novel visualization.
We interferometrically constrain often problematically degenerate parameters,
inclination and inner disk radius, allowing us to focus on the structure of the
wind, magnetosphere, and inner gaseous disk in radiative transfer models. Over
all timescales sampled, the strongest variability occurs within the blueshifted
absorption components of the Balmer series lines; the strength of variability
increases with the cadence of the observations. Finally, high-resolution
spectra allow us to probe substructure within the Balmer series' blueshifted
absorption components: we observe static, low-velocity features and
time-evolving features at higher velocities. Overall, we find the observed line
morphologies and variability are inconsistent with a scaled-up T Tauri MA
scenario. We suggest that as magnetic field structure and strength change
dramatically with increasing stellar mass from T Tauri to Herbig Ae/Be stars,
so too may accretion and outflow processes.
