Total Solar Eclipse Path & Obscuration Map
Explore the precise corridor of totality sweeping from the Arctic through Greenland, Iceland, and Spain, along with obscuration coverage across Europe, Canada, and the United States.
Palma de Mallorca
Spain · EUSpectacular sunset totality over the Mediterranean horizon.
Why isn't a Solar Eclipse visible everywhere on Earth?
Unlike global phenomena or Auroras, a solar eclipse depends on an exact, narrow geometrical alignment producing a moving shadow cone.
Moon Shadow Geometry (Umbra vs Penumbra)
The Moon is much smaller than Earth (approx 1/4 size). When it passes in front of the Sun, its central shadow cone (the Umbra) is only ~100–300 km wide when it strikes Earth's surface. Only observers standing directly inside this tiny moving band experience 100% Total Solar Eclipse.
Partial Obscuration Fan (The Penumbra)
Surrounding the narrow totality path is a broader outer shadow (the Penumbra). Obscuration diminishes with distance from the centerline: Eastern Canada/US see 30%-90%, Western Europe sees 80%-99%, while areas outside the penumbra (Asia, South America, Australia) receive direct sunlight with 0% eclipse.
Solar Eclipse vs. Aurora Borealis
Auroras occur in Earth's upper magnetosphere when solar wind particles collide with atmospheric gases over high geomagnetic polar latitudes. Solar Eclipses are mechanical optical blockages of sunlight caused by orbital mechanics, projecting a localized shadow across Earth as it rotates.
The Moon's umbral shadow traverses the Earth surface at supersonic speed.
Maximum path diameter during peak totality over Scoresby Sund, Greenland.
Structured dataset ready to incorporate future eclipse paths and global coordinates.
Never look directly at the Sun without proper ISO 12312-2 certified solar eclipse glasses. Never view partial phases with the naked eye, binoculars, or telescopes without ISO 12312-2 certified solar filters.