Aurora Activity
Space weather data for aurora chasers
Aurora Score
Conditions not suitable. Overcast, daylight, or quiet space weather.
Insufficient live data to produce a reliable score.
▲ activity.selectedLocation.demoScore
Space Weather Charts
Indicative demo data — live data coming soon
Kp Index History
Planetary K-index · Storm threshold at Kp 5
Unavailable
Solar Wind Speed
Activity threshold at 400 km/s
Unavailable
IMF Bz / Bt
nT · Southward Bz favours aurora
Unavailable
Solar Wind Density
Protons/cm³
Unavailable
Aurora Visibility
Pick a location to see your visibility
Current Space Weather
Kp Forecast (7h)
Kp forecast: Now: Kp 2, +1h: Kp 2.3, +2h: Kp 2.7, +3h: Kp 2.3, +4h: Kp 2, +5h: Kp 1.7, +6h: Kp 1.3
Geomagnetic Indices
Storm context for the current Kp value. The G-scale maps Kp to NOAA's geomagnetic storm severity; Ap is the daily activity average, and Max Kp 24h shows the highest 3-hour Kp seen in the last day.
Dst (storm intensity) is not shown — there is no free, real-time, browser-friendly Dst feed currently in use.
OVATION Aurora Model
NOAA's short-term aurora forecast model. Hemispheric Power is the total energy deposited into each polar region by precipitating particles — values above ~50 GW correlate with bright, mid-latitude-visible aurora. Updates every 5 minutes from the OVATION-Prime model.
Hemispheric Power — last 24h
24h · 5 min cadenceUnavailable
Sudden jumps between adjacent points are genuine OVATION model run updates, not data errors.
Sun at a glance
F10.7 Radio Flux
The solar radio flux at 10.7 cm — a reliable daily measure of the Sun's overall activity, closely tracking sunspot number and UV output. Measured from the ground at Penticton, Canada.
Flux trend
45 daysUnavailable
Typical range ~50–300 s.f.u. across a solar cycle; higher means a more active Sun.
Sunspot Regions
SDO · HMI intensitygram (flattened). Dark spots are the sunspot regions listed here.
Active regions on the Sun's surface — the sources of flares and CMEs. Larger, magnetically complex regions (β-γ-δ) are the most likely to erupt. Updated daily by NOAA SWPC.
Unavailable
Active regions on the Sun's surface — the sources of flares and CMEs. Larger, magnetically complex regions (β-γ-δ) are the most likely to erupt. Updated daily by NOAA SWPC.
Unavailable
SDO · HMI intensitygram (flattened). Dark spots are the sunspot regions listed here.
Solar Imagery
Real-time views of the Sun across different wavelengths and instruments. Each channel reveals a different layer of solar activity.
Click to enlarge
SDO · AIA 193 Å
1.25 MK corona. Dark regions are coronal holes — openings in the Sun's magnetic field where high-speed solar wind escapes. A hole facing Earth can drive geomagnetic activity, and aurora, 2 to 4 days later.
Coronagraph Views
Coronagraphs block out the bright solar disk to reveal the faint corona around it — the volume where coronal mass ejections (CMEs) are first seen propagating into space.
Click to enlarge
SOHO · LASCO C3
SOHO outer coronagraph (3.7 to 30 solar radii). The wider field follows CMEs further out; planets and bright stars regularly transit the field of view.
GOES Radiation
GOES-18 satellite measurements of X-ray flux from the Sun and energetic protons reaching Earth. Strong X-ray flares can disturb the ionosphere within minutes; proton storms can degrade GPS and pose radiation risk above 60° latitude.
X-ray flux — last 24h
24h · 0.1–0.8 nmUnavailable
Y-axis steps mark flare class boundaries (A → X). Each step represents a 10× increase in flux.
Recent flares — last 24h
Unavailable
Coronal Mass Ejections
Coronal mass ejections (CMEs) are massive eruptions of plasma and magnetic field from the Sun's corona. Earth-directed CMEs can drive significant geomagnetic storms 1 to 4 days after launch.
Local Weather Report
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Sun, Moon & Darkness
Data Sources
| Source | Updated | Status |
|---|---|---|
NOAA SWPC (opens in new tab) Kp index, solar wind, IMF Bz, aurora oval | — | ○ No data |
Nightcompass Weather Core (opens in new tab) Cloud cover, temperature, wind, visibility | — | ○ No data |
NASA DONKI (opens in new tab) Coronal mass ejection observations and analyses · ~few times/day | — | ○ No data |
OpenStreetMap · Protomaps (opens in new tab) Base map tiles | — | ● Static |
NASA Black Marble (opens in new tab) Light pollution / Bortle sky quality (VNP46A4) | — | ● Static |
Data sources are tracked for cost, licensing, attribution, and privacy requirements before production use.
Solar Wind Source
NOAA SWPC routes from active L1 monitors (ACE, DSCOVR, SOLAR-1, IMAP I-ALiRT). The operational spacecraft is selected upstream and not surfaced in the feed.
IMF Magnetic Field
Bz, Bt, Bx, By components — 1-minute cadence.
Solar Wind Plasma
Speed, density, temperature — 1-minute cadence.
Fresh ≤ 15 min · Delayed 15–60 min · Stale > 60 min.