last update
00:45 UTC
SFI: 80 | Ap index:  4  | Kp index:  0  ( n\a @--:--,  n\a @--:--)| X-ray flux:  n\a 
SW: Density= 1.2 p/cm3 | Speed= 342.5 km/s | Temp=33(x1000)K
IMF: Bx=-2.4nT | By=2.8nT | Bz= 1.3 nT | Bt= 3.9 nT | Lat= 19.1 ° | Lon=129.8°
Sunspots: 12 | Area: 130 10-6/Hemi | New regions: 0
[i]X-ray flares: C=0 M=0 X=0 | Optical flares: M1=0 M2=0 M3=0 | Sub-flares=0
Live data from the Geostationary Operational Environmental Satellite(s) (GOES)
X-ray flux

Measured by the GOES satellites (current satellite(s): GOES-16 (GOES-R)). 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 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 >=0.8 MeV/>=0.8 MeV and >=2 MeV/>=2 MeV at GOES-16 (75W). 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 (75W). The GOES‐R 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.


The Solar Ultraviolet Imager (SUVI) is a telescope that monitors the sun in the extreme ultraviolet wavelength range. By observing the sun, SUVI is able to compile full disk solar images around the clock. It replaces the GOES Solar X-ray Imager (SXI) instrument and represents a change in both spectral coverage and spatial resolution over SXI.

GOES-16 (primary)
Latest image from GOES-16 SUVI 94Å Latest image from GOES-16 SUVI 131Å Latest image from GOES-16 SUVI 171Å Latest image from GOES-16 SUVI 195Å Latest image from GOES-16 SUVI 284Å Latest image from GOES-16 SUVI 304Å
94Å (9.4nm)
131Å (13.1nm)
171Å (17.1nm)
195Å (19.5nm)
284Å (28.4nm)
304Å (30.4nm)
Latest image from GOES-17 SUVI 94Å Latest image from GOES-17 SUVI 131Å Latest image from GOES-17 SUVI 171Å Latest image from GOES-17 SUVI 195Å Latest image from GOES-17 SUVI 284Å Latest image from GOES-17 SUVI 304Å
GOES-17 (secondary)


SXI (superseded by SUVI)

The GOES 12 through 15 spacecraft each carry a sophisticated Solar X-ray Imager to monitor the Sun’s X-rays for the early detection of solar flares, coronal mass ejections, and other phenomena that impact the geospace environment. This early warning is important because travelling solar disturbances affect not only the safety of humans in high-altitude missions, such as human spaceflight, but also military and commercial satellite communications. In addition, coronal mass ejections can damage long-distance electric power grids, causing extensive power blackouts.

SXI videos

Latest 27 days: GOES 13 | GOES 14 | GOES 15
Latest 14 days: GOES 13 | GOES 14 | GOES 15
Latest 3 days: GOES 13 | GOES 14 | GOES 15

SXI Raw images: GOES 13 | GOES 14 | GOES 15
Current X-ray image of the Sun

Additional data

Kp 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). Kp indices of 5 or greater indicate storm-level geomagnetic activity.
Current Kp index plot
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.

D region absorption map
1dB ABS | 5MHz | 10MHz | 15MHz | 20MHz | 25MHz | 30MHz


Strongest X-ray solar flares recorded


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
* 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.

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