M Dwarfs, predominant among stars, offer a promising path for discovering Earth-size exoplanets due to their smaller sizes. Yet, their intense magnetic activity poses challenges for exoplanet detection and characterization, with active regions mimicking planetary signals in radial velocity and transmission spectroscopy. Understanding M dwarf magnetic activity, from internal dynamos to surface starspots, is vital for advancing exoplanet research. We monitored Hα, Hβ, Hγ and Hδ emission lines in 14 M Dwarfs to study short-term variability and emission sources. The sample consists of fully convective M Dwarfs at various evolutionary states, including young stars, T Tauri stars, and main sequence stars, as well as binaries and single stars. Spectra were obtained using the MDM Observatory's Ohio State Multi-Object Spectrograph on the 2.4m Hiltner Telescope, combined with TESS photometry to investigate evolving spot morphology and rotation periods. Sporadic short-term variability (equivalent width differences around -1 angstroms) in Balmer lines was observed in some stars, occurring on timescales (~ 15-60 min) much shorter than stellar rotation periods. In this poster, we quantify the type of variability we are seeing but also how its similar or different between each Balmer line. We also re-examine the amplitude-activity relation.