--
Kp Index
G0
G-Scale
Geomagnetic Activity
-- nT
Bz (IMF)
--- km/s
Solar Wind Speed
--- /cm³
Proton Density
-- min
--- km
DSCOVR to Earth

Recent Major Solar Flares (M & X Class)

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Bz (nT)
GOES Magnetometer Hp (nT)
Solar Wind Speed (km/s)
Proton Density (/cm³)
Bx (nT)
By (nT)
Bt (nT)
Temperature (K)
GOES Proton Flux
Low Energy Protons (ACE EPAM)

Experimental Graphs

US Mid-Latitude Aurora Favorability
US High-Latitude Aurora Favorability

Current Aurora Conditions - United States

US Mid-Latitude Aurora Stats

Based on averaged data points
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Bz: -- nT
Solar Wind: -- km/s
Density: -- p/cm³

US High-Latitude Aurora Stats

Based on averaged data points
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Bz: -- nT
Solar Wind: -- km/s
Density: -- p/cm³

These aurora favorability algorithms are experimental and under active development.

Interplanetary Magnetic Field Components

Active Spacecraft IMF (24 Hours)
IMF Clock Angle
IMF Cone Angle
Epsilon Parameter
The Epsilon parameter quantifies the energy coupling between solar wind and Earth's magnetosphere. Higher values indicate more efficient energy transfer, often leading to increased geomagnetic activity and aurora visibility.

Typical Values:
• Low: <0.5 GW
• Medium: 0.5-2 GW
• High: 2-10 GW
• Very High: >10 GW
Newell Coupling Function
The Newell Coupling Function measures the solar wind-magnetosphere coupling efficiency based on solar wind velocity, magnetic field strength, and clock angle. It's a key predictor of geomagnetic disturbances.

Typical Values:
• Low: <1000 m/s·T
• Medium: 1000-5000 m/s·T
• High: 5000-15000 m/s·T
• Very High: >15000 m/s·T
IMF Turnaround Events
IMF Persistence Timeline
Shows the duration of southward IMF Bz intervals. Longer periods of southward Bz allow more solar wind energy to enter the magnetosphere, increasing aurora potential.

Typical Durations:
• Low: <30 minutes
• Medium: 30-120 minutes
• High: 2-6 hours
• Very High: >6 hours
IMF Variability Index
Measures rapid fluctuations in the interplanetary magnetic field. High variability can indicate turbulent solar wind conditions that may enhance magnetosphere-ionosphere coupling.

Typical Values:
• Low: <2 nT
• Medium: 2-5 nT
• High: 5-15 nT
• Very High: >15 nT
Plasma Beta (β)
Alfvén Wave Activity
Alfvén waves are magnetic field oscillations in the solar wind. High wave activity can enhance energy transfer processes and contribute to magnetospheric heating and particle acceleration.

Typical Activity Levels:
• Low: <0.1 (relative units)
• Medium: 0.1-0.5
• High: 0.5-2.0
• Very High: >2.0
IMF Shear Angle
3D IMF Hodogram (Bx, By, Bz)
A hodogram is a 3D visualization showing how the interplanetary magnetic field (IMF) components Bx, By, and Bz change over time, with each point connected in chronological order.

Axes:
• Bx: Sun-Earth direction component
• By: Dawn-Dusk direction component
• Bz: North-South direction component

Key Patterns:
• Tight Clusters: Stable magnetic field
• Large Loops: Magnetic field rotations
• Linear Trends: Gradual field changes
• Bz < 0 (below center): Southward IMF, favors aurora

Navigation:
• Mouse drag to rotate view
• Scroll to zoom in/out
• Different time ranges show different scales of variability
Time Range:
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General Space Weather

SDO AIA 171 Å
SDO AIA 171 Å
SDO AIA 304 Å
SDO AIA 304 Å
SDO AIA 211 Å
SDO AIA 211 Å
SDO HMI Magnetogram
SDO HMI Magnetogram
SOHO LASCO C2
SOHO LASCO C2
SOHO LASCO C3
SOHO LASCO C3
STEREO-A COR2
STEREO-A COR2
CCOR1 Coronagraph
CCOR1 Coronagraph
SUVI Coronal Holes (195 Å)
SUVI Coronal Holes 195 Å

Current Active Regions

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Data refreshes automatically every 30 minutes.

Recent Solar Flares

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SUVI Full Sun (131 Å)
SUVI Full Sun 131 Å
GOES X-Ray Flux (6-Hour Timeline)
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WSA-ENLIL Model

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All data provided by NOAA Space Weather Prediction Center (SWPC)

Aurora Favorability Algorithms

How It Works

These experimental algorithms analyze real-time space weather data to estimate aurora visibility potential for different US latitude zones. The calculations combine multiple parameters including:

  • Interplanetary Magnetic Field (Bz) orientation and strength
  • Solar wind speed and density
  • Geomagnetic activity levels (Kp index)
  • Magnetometer deflections and substorm detection
  • IMF clock angle and coupling functions

Mid-Latitude Algorithm

Optimized for the northern US states (40-55°N), this algorithm requires strong southward Bz (below -8 nT) and elevated geomagnetic activity. It heavily penalizes quiet conditions and positive Bz values, as mid-latitude aurora requires significant geomagnetic disturbance.

High-Latitude Algorithm

Designed for Alaska and far northern regions (55°+ N), this uses different physics including cusp precipitation, EMIC waves, and polar cap dynamics. It's more responsive to moderate activity but still requires favorable conditions for significant aurora.

⚠️ Experimental Status

These algorithms are actively being tested and refined. Predictions should be used as general guidance only and combined with other aurora forecasting tools. Actual visibility depends on local weather, light pollution, and exact geomagnetic conditions at your location.

Aurora Latitude Zones in the United States

High-Latitude (55°+ N)

Northern Alaska including Fairbanks, Barrow, and the Arctic coast. Aurora visibility depends on solar wind conditions, Bz orientation, and local weather. These regions see aurora most frequently due to their proximity to the auroral oval.

Mid-Latitude (40-55° N)

Northern US states and major cities including Seattle, Minneapolis, Chicago, Detroit, Boston, and New York City. Aurora possible during geomagnetic storms when strong negative Bz combines with high solar wind speed and density.

Low-Latitude (Below 40° N)

Southern US including cities like Los Angeles, Phoenix, Dallas, Atlanta, and Nashville. Aurora extremely rare, only visible during exceptional geomagnetic storms with perfect alignment of space weather conditions.

Aurora visibility map showing magnetic latitude zones
Map from SpaceWeatherLive.com