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🌞 Solar Flare Eruption: Magnetic Reconnection & GOES Class (2D)

2D solar-flare lab: two sheared magnetic-loop arcades store free energy (E ∝ B²·V), reconnection releases it into a CME-like ejection whose speed follows straight from energy conservation, and a live GOES A/B/C/M/X class is derived from the modeled peak X-ray flux.

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This 2D companion drives the eruption from real magnetic-energy bookkeeping instead of a scripted explosion: two sheared, opposite-polarity loop arcades store free energy E ∝ B²·V, an Alfvén-speed-scaled reconnection rate sets how fast that energy is released, the CME's ejection speed comes straight from energy conservation on the freed kinetic energy, and a modeled peak X-ray flux is classified on the real GOES A/B/C/M/X scale — so field strength, loop shear and active-region size all visibly change both the eruption and its class, not just its color.

⚙ Under the hood

Free energy density u_free = (B·sinδ)²/(2μ0) is multiplied by an active-region volume L³ and a reconnection-efficiency fraction to get the energy released this event. A Petschek-type outflow (0.1·Alfvén speed) sets the reconnection timescale; 30% of the released energy becomes the CME's kinetic energy, giving its ejection speed from v = √(2·KE/m); a small fraction of the radiated remainder lands in the GOES soft X-ray band and is classified against the real A/B/C/M/X flux thresholds.

solar flaremagnetic reconnectionGOES classificationcoronal mass ejectionmagnetic energy densityalfvén speed

2D · HTML5 Canvas 2D · 60 FPS target · runs fully client-side, no install