GloTEC

Comparison page for GloTEC animations

The current operational GloTEC CONOPS uses a 10-minute cadence, 15-minute latency, and a 10-minute observation window for both ground-based and RO observations, centered on the analysis tag time. The current operational CONOPS with 15-minute latency prevents the usage of most of the RO data due to the data latency. To improve model accuracy through ingesting more RO measurements, the new experimental CONOPS configuration shown on this page retains the 10-minute cadence but uses a 30-minute latency. Ground-based TEC is ingested over a 10-minute window, whereas RO data are ingested over an expanded 30-minute window extending from 20 minutes prior to 10 minutes after the analysis tag time. Two versions of the new experimental CONOPS are shown here. One version assimilates TEC data from ground-based receivers and COSMIC-2 radio occultation TEC data (left column). The other version uses the same ground-based and COSMIC-2 data, and adds the real-time PlanetiQ radio occultation TEC data acquired through NOAA’s Commercial Data Program (right column). The PlanetiQ RO data comes from the satellites GNOMES-4 and GNOMES-5. Both satellites are in sun-synchronous orbit. GNOMES-4 orbits at 10LT and 22LT. GNOMES-5 orbits at 11LT and 23 LT. PlanetiQ data provides polar coverage in these specific local time sectors.

 

Contact tzu-wei.fang@noaa.gov with questions or feedback

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New experimental CONOPS

SOLAR-1

This is a test page for TLV for solar1 data

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CCOR1-DIFF Coronagraph

Imagery from the Compact Coronagraph (CCOR) instruments will be used by the SWPC Forecast Office to characterize activity in the outermost part of the Sun’s atmosphere known as the corona

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CCOR-2 Coronagraph

Imagery from the Compact Coronagraph (CCOR) instruments will be used by the SWPC Forecast Office to characterize activity in the outermost part of the Sun’s atmosphere known as the corona

Imagery from the Compact Coronagraph (CCOR) instruments will be used by the SWPC Forecast Office to characterize activity in the outermost part of the Sun’s atmosphere known as the corona. This includes monitoring data for transient events like coronal mass ejections (CMEs), as well as monitoring the impacts the corona has on the steady stream of plasma, referred to as the solar wind, emanating from the Sun. Ultimately, information derived from CCOR images will be used as inputs to the WSA-Enlil model to forecast the impacts of CMEs and the solar wind on Earth.

Space Weather Impacts On Climate
Electric Power Transmission
HF Radio Communications
Satellite Communications
Satellite Drag

The Compact Coronagraph-1 (CCOR-1), will image the Sun in the visible wavelength range from 480nm to 730nm. In order to image the much fainter corona, the CCOR-1 instrument will use an occulting disk to block light originating from the much brighter photosphere of the Sun. As a result, the field of view for CCOR-1 will span from 3.7 solar radii out to 17 solar radii with a spatial resolution of ~50 arcseconds. CCOR-1 is one of several instruments mounted on the Sun-Pointing-Platform of the Geostationary Operational Environmental Satellite-U (GOES-U). The GOES-U satellite launched on June 25th. On July 7th, GOES-U reached geostationary orbit and was officially renamed GOES-19 where it is currently operating. More detailed information on the CCOR-1 instrument is available here

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Solar Cycle Progression Update (Experimental Interactive Charts on VPC)

Updated solar cycle charts displaying new 2024 prediction for solar-cycle 25. Running in Highcharts

The observed and predicted ​Solar Cycle is depicted in Sunspot Number in the top graph and F10.7cm Radio Flux in the bottom graph.

In both plots, the black line represents the monthly averaged data and the purple line represents a 13-month weighted, smoothed version of the monthly averaged data. The slider bars below each plot provide the ability to display the sunspot data back to solar cycle 1 and F10.7 data back to 2004.

The predicted progression for the current solar cycle (Cycle 25) is given by the magenta line, with associated uncertainties shown by the shaded regions.  This prediction is based on a nonlinear curve fit to the observed monthly values for the sunspot number and F10.7 Radio Flux and is updated every month as more observations become available.  The shaded regions show the uncertainty in the prediction, obtained by applying the same prediction method to previous cycles at the same stage in each cycle.  In particular, the three shades show the first three quartiles (25, 50, and 75%) of the deviations from previous predictions.

This should be interpreted as follows.  There is roughly a 25% chance that the smoothed sunspot number will fall within the darkest shaded region at a particular time in the future.  Similarly, there is a 50% chance the smoothed sunspot number will fall in the medium-shaded region and a 75% chance it will fall in the lightest of the shaded regions.

These plots, like many on the SWPC website, are interactive.

  • Mousing your cursor over the plots will display the data values applicable to the date the cursor is over.
  • Left clicking on the data and holding while you drag will define a zoom window.
  • Use the buttons above each plot to return to the default zoom showing the current cycle or to show the entire available data set.
  • There is also an option to toggle the solar cycle numbering on/off.
  • Beneath each main plot window, the entire time series is shown and you can click/hold on either side of the blue shaded region to expand or contract the zoom window or if you click/hold on the blue shaded region itself, you can slide it to anywhere in the time series.
  • A drop down menu above and to the right of each plot allows you to PRINT, or download PNG, PDF, or SVG format images of the associated plot
  • Another drop down menu in the lower left to allows the user to plot the prediction made for Solar Cycle 25 by an international NOAA/NASA/ISES Panel in 2019, as well as the stated uncertainty in this prediction. 

Note that both the updated prediction and the 2019 NOAA/NASA/ISES Panel prediction apply only to Solar Cycle 25.  Solar Cycle 26 is expected to begin some time between January 2029 and December 2032.  We do not yet produce a prediction for Solar Cycle 26.  

Solar cycle predictions are used by various agencies and many industry groups. The solar cycle is important for determining the lifetime of satellites in low-Earth orbit, as the drag on the satellites correlates with the solar cycle, especially as represented by F10.7cm. A higher solar maximum decreases satellite life and a lower solar maximum extends satellite life. Also, the prediction gives a rough idea of the frequency of space weather storms of all types, from radio blackouts to geomagnetic storms to radiation storms, so is used by many industries to gauge the expected impact of space weather in the coming years.

The solar cycle prediction shown here is based fitting the observed data to a nonlinear function that reflects the average shape of solar cycles and that takes into account the observed tendency for stronger cycles to rise faster than weaker cycles.  Different curves are used to fit the International Sunspot Number and the F10.7 radio flux.    Uncertainties are based on applying the same prediction method to previous Solar Cycles, at the same point in each cycle, and then calculating the difference between the predicted and the observed smoothed monthly values.   For further technical details, please consult the validation document.

The 2019 Panel prediction comes from an international Panel that was convened in 2019 by NOAA, NASA and the International Space Environmental Services (ISES) for the express purpose of predicting Solar Cycle 25. After an open solicitation, the Panel received nearly 50 distinct forecasts for Solar Cycle 25 from the scientific community. Prediction methods include a variety of physical models, precursor methods, statistical inference, machine learning, and other techniques. The prediction released by the panel is a synthesis of these community contributions.  The Prediction Panel predicted Cycle 25 to reach a maximum of 115 occurring in July, 2025. The error bars on this prediction mean the panel expects the cycle maximum could be between 105-125 with the peak occurring between November 2024 and March 2026.  The updated prediction can be considered as a recalibration of the 2019 Panel prediction based on new observational data.

The original version of the Solar Cycle 25 prediction, released in 2019, only showed the baseline NOAA/NASA/ISES Panel prediction.   In February 2023, the Sunspot Number and F10.7 radio flux plots were modified to show the full range of the 2019 Panel prediction, taking into account expected uncertainties in the cycle start time and amplitude.

In October 2023 the updated prediction for Solar Cycle 25 was made available to the public as an experimental product on the Space Weather Prediction Testbed.  After a period of feedback from SWPC customers and the general public, the updated prediction was made available on this web site in  February 2025, replacing the 2019 Panel prediction.  However, the Panel prediction can still optionally be displayed using the drop down menus.

GOES SUVI Flare Location Product

GOES Solar Ultraviolet Imager (SUVI) Automated Flare Location Product

The GOES Solar Ultraviolet Imager (SUVI) Flare Location Product reports the latest solar flare location for SUVI’s “flaring” spectral channels (94Å and 131Å) in Heliographic Stonyhurst coordinates.

Do you have feedback about this product? Provide it here.

The GOES Solar Ultraviolet Imager (SUVI) is NOAA's operational solar extreme-ultraviolet (EUV) imager. This telescope allows forecasters to monitor the Sun’s hot outer atmosphere, or corona. Observations of solar EUV emission aids in the early detection of solar flares, coronal mass ejections (CMEs), and other phenomena that impact the geospace environment.

The real time SUVI flare location product reports flare locations for the SUVI “flaring” spectral channels (94Å and 131Å) with a 4 minute cadence. Graphical products show flare locations in the Heliographic Stonyhurst coordinate system for the most recent flare location. The SUVI Flare Location JSON data service also includes the flare location in R-theta, and pixel coordinate systems.

The SUVI Flare Locations are determined from the SUVI Thematic Map and, for each distinct flaring region, the algorithm returns the intensity-weighted centroid that indicates the location of each flare. Locations when the GOES X-ray Sensor (XRS) Event Detection algorithm determines that a solar flare is in progress.

For further details, see the following links: 

NOAA NCEI archive of GOES Products and additional documentation

Example Jupyter Notebooks to Plot SUVI Flare Locations

Journal Article on Thematic Map Approach