Our magnetohydrodynamical wind tunnel simulation uses a time-dependent wind mimicking what a jellyfish galaxy experiences while orbiting a 1.1 × 10¹⁵ M_⊙ cluster. This figure shows the resulting ICM wind speed, ICM wind density, and ram-pressure. In the first 1 Gyr we have a ‘burn-in phase’, where the galaxy settles into an equilibrium. Shortly after 2.0 Gyr the galaxy crosses R₂₀₀ of the cluster, and 3.0 Gyr marks the closest passage to the centre, where the ram-pressure peaks.