Ударний шар, магнетон і перемикач, що запускає північне сяйво

A star that never stops exhaling

The Sun's corona is so hot (over a million kelvin) that the Sun's gravity cannot hold onto it: the plasma continuously accelerates outward as the solar wind, reaching roughly 300 to 800 km/s by the time it passes Earth’s orbit, carrying with it the Sun’s magnetic field frozen into the flow (a consequence of magnetohydrodynamics called flux freezing). Because the Sun rotates, that dragged-out field forms a spiral — the Parker spiral — and its north-south component, the interplanetary magnetic field (IMF) Bz, turns out to be the single most important number in space weather.

The bow shock: nature's supersonic shockwave

The solar wind moves faster than the fast magnetosonic wave speed in that plasma, so when it meets an obstacle it cannot just flow smoothly around — the information "there is an obstacle here" cannot propagate upstream fast enough. The result is a standing bow shock, analogous to the shockwave in front of a supersonic aircraft, sitting roughly 90,000 km sunward of Earth. Crossing it, the plasma abruptly slows, heats and compresses, and the flow becomes subsonic and turbulent in the magnetosheath just behind it.

The magnetopause: where two pressures balance

Deeper in, the solar wind's dynamic pressure pushes against Earth’s own magnetic field until the two balance at a boundary called the magnetopause. Its stand-off distance is set by pressure balance and is well described empirically by the Shue model (1997), which fits the boundary shape as a function of both solar wind dynamic pressure and IMF Bz:

r(θ) = r0 * (2 / (1 + cos θ))^α

r0 typically ≈ 10 Earth radii on the dayside under average conditions

r0 shrinks under high solar wind pressure or strongly southward Bz

α controls how quickly the boundary flares into the elongated nightside tail

Under calm conditions the dayside magnetopause sits near 10 Earth radii; during a strong solar storm it can be compressed to 6 or fewer, occasionally exposing geostationary satellites (at about 6.6 Earth radii) directly to the shocked solar wind.

r(θ) = r0 · (2 / (1 + cos θ))^α

r0 typically ≈ 10 Earth radii on the dayside under average conditions
r0 shrinks under high solar wind pressure or strongly southward Bz
α controls how quickly the boundary flares into the elongated nightside tail

Reconnection: the switch that lets energy in

Earth's dipole field points north at the dayside magnetopause. When the IMF carried by the solar wind is itself pointed south (negative Bz), the two oppositely directed field lines meet at the boundary and can break and reconnect — a process called magnetic reconnection that converts magnetic energy into particle kinetic energy and, crucially, opens a direct topological channel for solar wind plasma and energy to enter the magnetosphere. Northward IMF, by contrast, largely keeps the magnetosphere closed and quiet. This single sign flip in one number is why space weather forecasters watch Bz more closely than almost any other solar wind parameter.

Where the aurora comes from

Reconnection loads the magnetotail with energy that is later released explosively in a substorm, accelerating electrons and protons along magnetic field lines down into the upper atmosphere near the poles. There they collide with oxygen and nitrogen: oxygen produces the familiar green (557.7 nm) and, higher up, red (630 nm) emission, while nitrogen contributes blue and purple hues.

The oval of auroral activity expands to lower latitudes precisely when Bz has been strongly southward for an extended period — which is exactly the parameter this simulation lets you turn to trigger reconnection and watch particles precipitate toward the poles.

Frequently asked questions

Спробуйте наживо

Усе, що вище, працює прямо у вашому браузері — відкрийте Solar Wind і змінюйте параметри під час роботи. Нічого не встановлюється, нічого не завантажується на сервер, уся модель живе в одній вкладці.