Our physical picture for GRB 250702B. Panel (a) shows the geodesic orbit of the WD, where the red line represents our numerical result with a = 30 R_⊙, e = 0.97, M_BH = 1 × 10⁵ M_⊙, a_spin = 0.9, and ﹩{\theta }_{{\rm{\min }}}=0.12\,{\rm{rad}}﹩ (7^∘). The BH spin axis is indicated by the vertical black line. The orbit exhibits relativistic precession. Mass loss from the WD is not included in this calculation. Panel (b) illustrates an unobservable configuration. An accretion disk forms with its angular-momentum vector tilted by an angle θ_d with respect to the BH spin axis. As a result, the jet undergoes Lense–Thirring precession. If ∣θ_v,BH − θ_d∣ > θ_j, the jet does not intersect the line of sight, and the prompt emission remains unobservable. Panel (c) shows an observable configuration. If ∣θ_v,BH − θ_d∣ ≲ θ_j, the jet remains continuously observable throughout the Lense–Thirring precession.