IMPORTANT:
Core features of this service require your location to function properly.

You can enable the geo location feature in your browser or mobile device to access information more relevant for your location or view the service with the default location set to Whitehorse, Yukon Canada. :)

Aurora Geek Beta v.2

Pick Your Aurora Destination: See current conditions at another location!


Loading... your aurora forecast probability.
 

Your Aurora Data Dashboard

Welcome to the Aurora Geek data dashboard! Here we try to put every piece of aurora forecast data relevant to the current availability as we can. You'll find the information here is as real-time as possible. If enabled, this page uses geo location capabilities of your browser or mobile device to make the content of this page more relevant for you, where you are.

Where's the moon at?

Sunset
Solar Midnight
Sunrise

Solar Wind

Solar Wind Velocity

Why the solar wind velocity matters

The solar wind is a stream of charged particles from the Sun that interacts with Earth's magnetic field. When the solar wind is strong, it can trigger more intense auroras. When the solar wind is more energetic, it can cause disturbances in Earth's magnetosphere, resulting in more vibrant and dynamic auroras, often referred to as auroral substorms.

Particle Density

Why the solar wind particle density matters

Particle density in the solar wind refers to the concentration of charged particles, such as protons and electrons. Higher density increases the likelihood of interactions with Earth's magnetic field, amplifying auroral activity. Along with solar wind speed and magnetic field strength, particle density plays a key role in determining the intensity of the aurora.

Interplanetary Magnetic Field

Bz IMF Value

Why the magnetic field Bz matters

Interplanetary Magnetic Field (IMF) Bz is the vertical component of the interplanetary magnetic field. When the Bz is negative (southward), it allows for greater interaction with Earth's magnetic field, enhancing the likelihood of auroral displays. A negative Bz is often considered a key factor in triggering strong auroral activity.

Bt IMF Value

Why the magnetic field Bt matters

Interplanetary Magnetic Field (IMF) Bt is the total strength of the interplanetary magnetic field. Higher Bt values indicate a stronger magnetic field, which increases the potential for interactions with Earth's magnetosphere, often leading to more intense auroras when combined with favorable Bz conditions.

Hemispheric Power Index

The Hemispheric Power Index (HPI) is a measure of the total power in gigawatts (GW) being deposited into the Earth's upper atmosphere by charged particles from the solar wind, specifically in the auroral regions. It is derived from satellite observations of the auroral oval and gives an estimate of the energy available to produce auroras in each hemisphere.

What to look for? Keep an eye out for higher values. Above 20GW aurora borealis can be visible to the naked eye in nothern areas where aurora is common. Getting above 50GW and the lights will be more visible further south and above 100GW and it's party time.