Understanding how young stars gain mass is important because it affects our knowledge of the star and planet evolutionary process. Accretion onto Herbig stars is especially interesting because the precise mechanism by which they accrete mass is not well understood. As a result of accretion, young stars tend to show both photometric and spectroscopic variations attributed to accretion from the circumstellar disk, and when monitored over time, the H-alpha emission line traces variability in the mass accretion rate. In this study, we present time-series optical spectra from the Tull spectrograph on the McDonald Observatory Harlan J. Smith 2.7-m telescope of the young A0 Herbig Ae star, AB Aurigae (AB Aur). We quantified the variability of the H-alpha line over a range of timescales, spanning minutes to weeks to characterize the mass-flow geometry around the star. Results of this study reveal key details of the accretion behavior of AB Aur and provide insights into potential mechanisms by which young Herbig Ae stars accrete mass. EL acknowledges support from NSF REU grant AST-2244278 (PI: Jogee).