Geomagnetic Storm: Solar Wind Deflection (2D)

This 2D companion swaps the original's decorative particle swarm for a physically driven charged-particle model: it integrates the actual Lorentz force F = qv×B for a stream of solar-wind protons and electrons crossing Earth's equatorial dipole field, whose field strength falls off as B ∝ 1/r³ with distance from Earth. Protons and electrons curve in opposite senses under the same field — visible immediately as mirrored spiral trails — while a live readout tracks how many particles get trapped in the radiation-belt band, how many precipitate into the polar caps as aurora, and how many are simply deflected around the magnetopause, all driven directly by the speed, field-strength and density sliders rather than a fixed animation.