Current Data

GOES Solar Images and Particle Fluxes

GOES SUVI Instrument

GOES SUVI image at 19.5 nm (Fe XII) from the corona of the Sun, useful for viewing solar flares and coronal holes.

GOES SUVI image at 30.4 nm (He II) from the chromosphere, highlighting solar variability and active regions.

GOES Proton Flux

GOES satellite data on proton flux, showing the impact of high-energy particles on electronics and HF communication.

Detailed proton flux measurements used to assess space weather effects on geostationary satellites.

GOES Electron Flux

GOES proton particles >1 and >10 MeV and electron particles .5-.7 MeV observations measured at 5-minute cadences. The GOES electron flux indicates the intensity of the outer electron radiation belt. Electron flux can impact satellite drag and communications. GOES proton flux measures proton particles from the Sun to the Earth. Proton flux impacts space weather and GPS systems, HF radio communications, and satellite communications. Values increase in the proton flux during events like solar flares.

Differential electron flux data indicating outer radiation belt intensity at geostationary orbit.

Electron flux values providing insights into spacecraft surface charging risks and effects.

Solar Irradiance and Indices

Forecast Solar Indices

SET operationally provides these forecast solar indices for use by the JB2008 model. In addition to the legacy F10 proxy representing both the solar transition region and corona with bremsstrahlung and free-free electron processes, the remaining operational solar indices represent the combined energy from these sources: i) S10 is the 26-34 nm bandpass EUV chromospheric irradiance index; ii) M10 is the 160 nm FUV Schumann-Runge photospheric irradiance proxy; and iii) Y10 is the 121.6 nm Lyman-alpha chromospheric/transition region irradiance convolved with the 0.1–0.8 nm X-ray coronal irradiance. S10 represents the energy for O photoabsorption in the middle thermosphere (>180 km), M10 represents the energy for O₂ dissociation in the lower thermo- sphere (~110 km), and Y10 represents the energy for mesosphere and lower thermosphere H₂O chemistry (~90 km). F10 captures any remaining energy that is unresolved in atmosphere layers. All units are reported in solar flux units (sfu) of ×10^-22 W m^-2 Hz^-1.

X-ray shows X-ray flux on a 1-minute cadence. The Graph indicates the flare initiation the as well as the flare maximum and end.

GOES X-ray is used to track solar activity and solar flares. The bottom graph shows B the begin time of an X-ray event, M, the X-ray event maximum or peak Xray flux, C is the current X-ray event.

Forecast solar indices for use by the JB2008 model

Mg II c/w (Center-to-Wing Ratio) Measurement

The Mg II c/w (center-to-wing ratio) measurement has been an important input to solar irradiance models, and is one of the best chromospheric time series available for describing solar FUV/EUV irradiance variations from daily to solar cycle timescales. It is the basis for M10 index used in the JB2008 model. The Mg II c/w is a relative photometric measurement at 280 nm between the Mg II h and k lines. Because it is based on the ratio of the lines, and not to an absolute calibration, it is much less susceptible to instrument degradation. Continuous daily values are available from late 1978, covering nearly five solar cycles. In many ways, compared to sunspots and the F10.7 2800 MHz data, it is a superior index to solar irradiance variability and space weather applications because it can accurately describe chromosphere variability on time scales ranging from a solar rotation (27 days) to the 11-year solar cycle, and, unlike F10.7, it describes the solar FUV variability that directly affects the Earth’s lower thermosphere. Additional information for data users can be found at SET Operational Mg II c/w data: Information for data users.

A detailed graph depicting Mg II c/w variability over several solar cycles.

Geomagnetic Indices (Dst)

Geomagnetic storms are measured using the Dst index, which tracks the magnetospheric ring current’s strength and its depression of Earth’s magnetic field. SET’s Anemomilos Dst forecast predicts storm impacts using solar flare data and storm indicators, offering insights several days ahead.

Geomagnetic storms are measured by the Disturbance storm time (Dst) index, which reflects the strength of the magnetospheric ring current caused by substorms and storms. As electrons drift from the magnetotail to the dawn sector, a current system forms, depressing Earth’s magnetic field. Dst values are measured in nT and are typically negative during storms. SET’s Anemomilos Dst index forecasts storm impacts using solar flare magnitude, location, and energy to predict geomagnetic activity several days in advance.

SET’s coronal mass ejection (CME) arrival forecast displays the Sun (yellow) and Earth (blue) icons from a top-down view of the ecliptic plane. The Sun’s west limb is at the top. Colored dots represent the CME flux rope at 12-hour intervals, with polarity (southward or northward Bz) estimated from solar polar field configurations. The Sun-Earth line is a dotted line connecting the icons. Timing, magnitude, and duration are detailed in the legend, while the bottom color bar shows the solar X-ray flare index (Xhf) with background values removed. The flare’s solar longitude and latitude are marked on the Sun icon.

DSCOVR Solar Wind

DSCOVR Solar Wind Data

Solar wind speed data from DSCOVR at the L1 point shows variations over the past 6 days, ranging from typical speeds (350-450 km/s) to high-speed streams and coronal mass ejections.

Solar wind electron density data over the past 6 days highlights its role in geomagnetic storm coupling and particle injection into the Earth’s magnetosphere.

Solar wind temperature data from DSCOVR illustrates its influence on geomagnetic storm coupling with Earth’s magnetosphere.

The Bz component of the solar wind’s magnetic field affects geomagnetic storm intensity, with southward Bz coupling more strongly with Earth’s magnetosphere.

NAIRAS Effective Dose Rates

The NAIRAS model predicts atmospheric radiation exposure from galactic cosmic rays (GCR) and solar energetic particle (SEP) events. This show the NAIRAS prediction related to biological risk for the Northern Hemisphere at Altitude 5km or ~16,000 ft.

The NAIRAS model predicts atmospheric radiation exposure from galactic cosmic rays (GCR) and solar energetic particle (SEP) events. This show the NAIRAS prediction related to biological risk for the Northern Hemisphere at Altitude 11km or ~36,000 fit the average altitude for commercial airplanes.

The NAIRAS model predicts atmospheric radiation exposure from galactic cosmic rays (GCR) and solar energetic particle (SEP) events. This show the NAIRAS prediction related to biological risk for the Northern Hemisphere at Altitude 15km or ~49,000 ft.

The NAIRAS model predicts atmospheric radiation exposure from galactic cosmic rays (GCR) and solar energetic particle (SEP) events. This show the NAIRAS prediction related to biological risk for the Northern Hemisphere at Altitude 90km or ~300,000 ft.

GEOPOT08 Geosynchronous Charging at SDO (102W)

GEOPOT08 Geosynchronous Charging

Geosynchronous charging environments come from the Geosynchronous Plasma Environment Model (GEOPOT08). This shows the charging conditions for the shaded non-lit spacecraft surfaces. The charging environment is a serious concern for satellites orbiting near geosynchronous orbit (GEO)

Geosynchronous charging environments come from the Geosynchronous Plasma Environment Model (GEOPOT08). This shows the charging conditions for the sunlight spacecraft surfaces. The charging environment is a serious concern for satellites orbiting near geosynchronous orbit (GEO)

NOAA SWPC Ap

NOAA SWPC Ap Index

The Ap index provides a daily average level for geomagnetic activity. Every 3-hour K value is converted into a linear scale called the A-index the average from 8- daily A-values gives the Ap-index. Days with high geomagnetic values have a higher Ap-value.

Space weather data from SET’s operational systems, updated in real time.