Schematic representation illustrating how pulses form relying on simple geometric considerations based on the split-monopole configuration. Here, χ = 60° for illustrative purposes, but this picture applies for all inclinations (except the aligned and orthogonal rotators). In this diagram, the pulse P1 (P2) is emitted once the sheet 1 (respectively 2) rotating at the angular velocity of the star, Ω, overlaps with the fixed black dashed line, an iso-phase contour set by the observer. Three typical configurations are presented: (i) an equatorial view (α = π/2) leads to two symmetric pulses separated by ΔΦ = 0.5, (ii) an off-equator view within the striped wind region (α = π/2 − 0.8χ) where the pulses are asymmetric and separated by ΔΦ = 0.28 and contains significant emission in between (a bridge or third peak, green region), and (iii) the degenerate single pulse case (ΔΦ = 0) where the observer’s line of sight grazes the outer boundary of the stripes (α = π/2 − χ).