Aurora Academy

Become an Aurora Hunter.

From solar physics to the impact on Earth's atmosphere. Learn to read the data and forecast geomagnetic storms.

Kp4.3Demo

Bz−8.6 nTSOUTH

Solar Wind612 km/sHigh-Speed Stream

The Journey

From the Sun to Earth

Discover the path of solar energy through space to our atmosphere.

01/05

It all begins on the Sun. Enormous explosions called Coronal Mass Ejections (CMEs) hurl billions of tons of magnetized plasma into space.

RememberThe greater the solar activity (sunspots), the higher the chances of strong auroras.

Geomagnetic Expansion

Kp 0-3: Restricted oval. Quiet activity, visible mainly above the Arctic Circle (Tromsø, Lapland).

Indice Kp: 3

Kp 0Kp 5Kp 9

The color depends on the type of gas struck by solar particles and the altitude at which the collision occurs.

The densest region. Excited oxygen here emits the classic bright GREEN or yellow-green light, by far the most common auroral color.

Now that you know the theory, learn to read the indicators in our app so you never miss a storm.

Planetary Index

Indicates the extent of the auroral oval. Higher values mean auroras may be visible farther south.

Magnetic Field

When it points southward (negative), solar energy enters Earth's atmosphere on a massive scale.

Plasma Speed

Streams above 500 km/s compress the magnetosphere more strongly, triggering the display.

Monitor solar data in real time, receive geomagnetic storm notifications and use interactive cloud-cover maps to find clear skies.

Test yourself

1 / 3

Which parameter is essential for solar energy to quickly 'enter' our magnetosphere?