Magnetar Crust Seismology: Torsional Ringdown Modes

After a magnetar's giant flare cracks its rigid crust, the star doesn't just settle — it rings. This simulation renders the neutron star as a lattice of crustal patches over a glowing core and lets you excite real torsional shear-oscillation modes (ℓ = 2 through 6), the same standing waves inferred from the quasi-periodic X-ray oscillations seen after real giant flares such as SGR 1806-20 in 2004. Adjust the crust's shear rigidity and damping quality factor, trigger a starquake, and watch the mode frequency, ring-down amplitude and elapsed time update live as the exponentially-decaying oscillation propagates across the surface exactly as the governing shear-wave formula predicts.