Average line profile at both conjunctions (continuous line) is compared with the first (dash) and the last (dots) of the individual 5-spectrum averages of the same night, illustrating that the spectra at these orbital phases are all broader than near elongations. The significantly different profile at ⟨ φ ⟩ = 0.135 is caused by the presence of m₂ having moved from near the core of m₁’s absorption to its wing over the ~7 h that these observations lasted. The rapid motion is due to the fact that this phase is just after periastron.