Top: suite of panels at 12 keV varying θ_v ∈ {6°, …, 90°} and ϕ₀ ∈ {0°, …, 180°} with θ₀ = 18°, Δθ₀ = Δϕ₀ = 2°, M = 2.0 M_⊙, r_⋆ = 12 km, ﹩{B}_{p}^{{\rm{flat}}}=10﹩, α = 1/3, ﹩{m}_{e}{c}^{2}{{\rm{\Theta }}}_{{\rm{\max }}}=30﹩ keV, and η = 0, and splitting ⊥ → ∥∥ only. Bottom: attendant time-integrated snapshot spectra for each case. This demonstrates that geometric changes can lead to strong spectral and apparent luminosity variations. There is strong geometric and visibility enhancement of luminosity of bursts behind the NS, compared to those in the foreground that can occult high luminosity low-altitude regions of the burst. The high luminosity outlier θ_v = 20° and ϕ₀ = 180° is a result of surface grazing trajectories near the back and lensed polar footpoints that are strongly beamed along B.