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Polski☀️ Solar Wind & Magnetosphere Storm Simulator (3D)
Drive the solar wind's speed, density and interplanetary magnetic field, and watch Earth's magnetosphere compress, reconnect and light up the aurora in real time.
Earth sits inside a bubble carved out of the Sun's constant outflow of charged particles — the solar wind. This 3D companion turns that invisible tug-of-war into something you can steer directly: push the wind speed and plasma density up and the magnetopause (the boundary where Earth's magnetic field finally overpowers the wind) gets shoved inward, visible here as the wireframe shell and the dipole field-line cage compressing on the sunward side and stretching into a long magnetotail behind. Tip the interplanetary magnetic field (IMF Bz) southward and the field lines on the dayside reconnect with Earth's own field, opening a direct channel for solar-wind plasma to funnel down into the polar cusps — shown as particles bending toward the poles and the auroral rings lighting up green and red. A "Launch CME" button simulates a coronal mass ejection: a sudden jump in wind speed and a sharp southward Bz swing, the classic recipe for a major geomagnetic storm.
A hand-rolled Three.js scene streams solar-wind particles from a point Sun toward Earth along the Sun-Earth line. Each frame recomputes a Shue-style magnetopause standoff distance from dynamic pressure (density × speed²) and deforms the field-line cage and bow-shock mesh to match; particles whose impact parameter falls inside that boundary are either deflected around Earth (northward Bz) or funneled toward the poles (southward Bz, magnetic reconnection), driving the aurora-ring opacity. The Kp-index, storm class and aurora-latitude readouts use a simplified illustrative formula loosely inspired by empirical coupling functions — not a live forecast.
3D · Three.js / WebGL renderer · 60 FPS target · runs fully client-side, no install
Earth's magnetic field holds the solar wind back by pressure balance: the field's magnetic pressure pushes outward, the wind's dynamic pressure (which scales with density × speed²) pushes inward. Raise either one and the boundary where they balance — the magnetopause — moves closer to Earth.
Earth's own field points northward near the equator. When the interplanetary field arriving from the Sun points southward, the two fields are anti-parallel where they meet on the dayside, and they can reconnect — briefly merging and reconfiguring into open field lines that let solar-wind plasma stream directly into the polar upper atmosphere, where it excites the gases that glow as the aurora.
No — it's computed live from the sliders using a simplified formula loosely modeled on real coupling functions, purely to make the relationship between wind conditions and storm intensity tangible. It is not connected to any live space-weather feed.