Measurements of Hα and Hβ observations of the Be star 25 Ori, similar to Fig. 5. For Hα, the EW_V/EW_R ratio was calculated using the wings of Hα, as indicated in the middle-right panel (between -600 and -300 km s⁻¹ and +300 and +600 km s⁻¹, i.e., outside of v sin i). However, the same behavior is seen in Hα even when using the entire line profile. Similar behavior is seen in Hβ for EW_V/EW_R (calculated using the full line profile out to ±400 km s⁻¹), including a third epoch of EW_V/EW_R variations that are less evident in Hα. Top-right panel: Anticorrelation between TESS brightness and Hα emission strength.