# Reconexión Magnética y Generador de Arco Auroral

Modelo interactivo del viento solar a la magnetosfera a la aurora: arrastre el Bz del IMF, vea cómo se reconectan las líneas de campo, se forma el punto X y se enciende el óvalo auroral.

> Página canónica: https://elysiatools.com/es/visualizations/magnetic-reconnection-aurora

- **Categoría:** Physics

## Descripción general

Interactive solar-wind → magnetosphere → aurora model — distinct from the existing plasma-dispersion (a cold-plasma wave dispersion relation), casimir-effect (quantum vacuum), and kelvin-helmholtz-instability (a hydrodynamic shear instability); this is the only case showing magnetospheric field-line topology change driven by IMF Bz and the dayside reconnection that powers space weather and the aurora. The field model superposes a tilted magnetic dipole B_dip with moment along −z (so the dayside equatorial field points northward — the reason southward IMF is geoeffective), a Parker-spiral-projected uniform interplanetary magnetic field (IMF), and a Harris tail current sheet Bx = B_t·tanh(z/δ) confined to the nightside (x<−6 R_E) with plasma-sheet half-thickness δ≈0.8 R_E; the total field is sampled and its topology classified by RK4 field-line tracing in arc-length, distinguishing closed dipole lines from open polar-cap lines. An analytic X-point null forms on the +x subsolar axis where −M/x³ + Bz = 0, i.e. x* = (M/Bz)^(1/3), only for southward Bz. Reconnection is modeled at both ends of the speed spectrum: the Sweet–Parker slow collisional rate ε_SP = S^(−1/2) with layer thickness δ_SP = L/√S, versus the Petschek fast shock-mediated rate ε_P ≈ π/(8 ln S), where the Lundquist number S = V_A·L/η is computed from local plasma-sheet values — demonstrating why nature almost always picks the fast branch. The geoeffective reconnection electric field E_y = v_sw·|Bz| (southward only) drives the coupling; the Akasofu (1981) energy-input parameter ε = v_sw·B²·L₀²/μ₀ (L₀=7 R_E) and an empirical Kp proxy (monotone in P=v_sw·|Bz|, calibrated so quiet solar wind→Kp≈1 and superstorm→Kp≈9) quantify the magnetospheric response. The auroral oval follows a Feldstein–Starkov type boundary model: equatorward and poleward corrected geomagnetic latitudes as harmonic functions of magnetic local time (MLT) and Kp, with the characteristic midnight bulge and ~1.8°/Kp equatorward expansion; oval center and width are reported. Emission color follows the altitude taxonomy: a power-law deposition relation h(E₀) = 50 + 80·E₀^(−0.3) km maps electron characteristic energy to deposition altitude, and the dominant band is red O I 630 nm (>160 km, soft electrons), green O I 557.7 nm (95–160 km, the common aurora), or purple N₂⁺ (<95 km, hard electrons), reflecting collisional quenching of the long-lived red state at low altitude. Four visualization panels: (1) Magnetosphere meridional (x–z) cut with the Sun on the right, showing the traced closed (cyan) vs open (gold) field lines, the dashed magnetopause ellipse from the Shue (1997) subsolar standoff r₀=(11.4+0.013·Bz)·P_dyn^(−1/6), an animated solar-wind flow, a glowing Earth disc, the X-point marker with its out-of-page reconnection electric field, and animated convection dots riding the open lines. (2) Reconnection-layer zoom showing anti-parallel inflow field lines, Alfvénic outflow jets animated at the outflow speed, the Sweet–Parker sheet thickness δ_SP box, and the central X-line. (3) Auroral oval polar view from above the north magnetic pole, with the MLT clock (noon/midnight/dawn/dusk), latitude grid, the glowing oval ring filled with the emission color from E₀, and shimmering arcs circulating along it. (4) Emission altitude profile plotting the Gaussian deposition peak at h(E₀) against the color-coded red/green/purple altitude bands and their wavelengths. Adjustable parameters: IMF Bz (−20 to +20 nT, the master switch), solar-wind speed v_sw (300–900 km/s), density n (1–40 cm⁻³), dipole tilt (±30°), characteristic electron energy E₀ (0.3–30 keV, setting the aurora color), and resistivity log₁₀(η) (−3 to 0, driving the Lundquist number and the SP/Petschek contrast). Four scenario presets: Quiet (northward IMF, no reconnection), Active (southward, Kp≈4), Storm (Kp≈6), and Superstorm (Kp≈7, oval reaches mid-latitudes). Real-time diagnostics: regime classification, magnetopause standoff distance, reconnection E-field, Kp index, Lundquist S, both Sweet–Parker and Petschek ε (to compare directly), Alfvén outflow speed, X-point height, Akasofu ε power, deposition altitude and emission band, and the oval's equatorward latitude. Educational content covers the solar-wind→aurora causal chain, Earth's tilted dipole and why southward IMF is geoeffective, Sweet–Parker vs Petschek reconnection and the plasmoid fast-reconnection mechanism, the Kp index and Akasofu energy input, the altitude→color physics (O I 630/557.7 nm, N₂⁺, collisional quenching), and applications to space weather (power-grid/GPS/satellite threats), fusion-energy plasma disruptions, astrophysical reconnection (solar flares, pulsar wind nebulae, NASA MMS mission), and the human experience of aurora. Multi-language support (zh, en, es, fr, de, ru, pt).

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