https://sol24.net/data

X-ray flux
Measured by the GOES satellites (current satellite(s): GOES-16/GOES-18). Spikes are considered significant when they rise above the “M” (10^-5W/m²) level. The plot shows the solar X-ray output in the 1-8Å (0.1-0.8 nm) and 0.5-4.0Å (0.05-0.4 nm) passbands.

Proton flux
Current 5-minute averaged integral proton flux. At the moment the levels are measured by the SWPC GOES-16 or GOES-18 satellite. SWPC`s proton event threshold is 10 protons/cm²s^-1sr^-1 at ≥10 MeV.

Electron flux
Current 5-minute averaged integral electron flux. The plot shows flux with energies ≥2 MeV (GOES-16/GOES-18). The data in this plot is invalid during a significant proton event because of sensor contamination at the GOES spacecraft.

Magnetic field
Current 1-minute averaged parallel component of the magnetic field. Measured in nanoTeslas (nT) at GOES-16/GOES-18. The GOES spacecraft use hydrazine arcjet thrusters for periodic orbital maneuvers to maintain the desired geostationary location. During arcjet operation, the magnetometer measurements are corrupted by ~20 nT, which is significant relative to the typical 100 nT geomagnetic field magnitude at geostationary orbit.

K_p Index (estimated)
The Estimated 3-hour Planetary K index is derived at the NOAA SWPC using data from ground-based magnetometers in Boulder (Colorado), Chambon la Foret (France), Fredericksburg (Virginia), Fresno (California), Hartland (UK), Newport (Washington), Sitka (Alaska) and Jeju (Korea). K_p indices of 5 or greater indicate storm-level geomagnetic activity.

D Region Absorption Predictions

Conditions in the D region of the ionosphere have a dramatic effect on high frequency (HF) communications and low frequency (LF) navigation systems. The global D Region Absorption Predictions (D-RAP) depicts the D region at high latitudes where it is driven by particles as well as low latitudes, where photons cause the prompt changes.

1dB ABS | 5MHz | 10MHz | 15MHz | 20MHz | 25MHz | 30MHz

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Strongest X-ray solar flares recorded

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RANK              DATE                CLASS
--------------------------------------------
  1             04-11-2003              X28+*
  2             02-04-2001              X20.0
  2             16-08-1989              X20.0
  3             28-10-2003              X17.2
  4             07-09-2005              X17.0
  5             06-03-1989              X15.0
  5             11-07-1978              X15.0
  6             15-04-2001              X14.4
  7             24-04-1984              X13.0
  7             19-10-1989              X13.0
  8             15-12-1982              X12.9
  9             06-06-1982              X12.0
  9             01-06-1991              X12.0
  9             04-06-1991              X12.0
  9             06-06-1991              X12.0
  9             11-06-1991              X12.0
  9             15-06-1991              X12.0
  10            17-12-1982              X10.1
  10            20-05-1984              X10.1
  11            29-10-2003              X10.0
  11            25-01-1991              X10.0
  11            09-06-1991              X10.0
  12            09-07-1982              X9.8
  12            29-09-1989              X9.8
  13            22-03-1991              X9.4
  13            06-11-1997              X9.4
  14            24-05-1990              X9.3
  14            06-09-2017              X9.3
  15            05-12-2006              X9.0  
  15            06-11-1980              X9.0 
  15            02-11-1992              X9.0
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* Taking a different route, researchers from the University of Otago used radio wave-based measurements of the x-rays’ effects on the Earth’s upper atmosphere to revise the flare’s size from a merely huge X28 to a “whopping” X45, say researchers Neil Thomson, Craig Rodger, and Richard Dowden.

Courtesy of NOAA/SWPC.