Solar-wind particles enter from the left. Earth's equatorial dipole field (B ∝ 1/r³, out of plane) bends them via the real Lorentz force F = qv×B — watch protons and electrons gyrate in opposite senses and pile up at the magnetopause.
Active particles0
Storm index (Kp)0.0
Trapped in belt0
Aurora hits0
Avg gyroradius0
Deflected (shock)0
Higher speed + weaker field compresses the magnetopause and raises the storm index. A field-line grid shows the dipole; the pale ring marks the trapped radiation belt.