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| Warnings and Alerts | |
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Issue Time: 2026 Mar 22 1042 UTC
WARNING: Geomagnetic K-index of 7 or greater expected Valid From: 2026 Mar 22 1041 UTC Valid To: 2026 Mar 22 1500 UTC Warning Condition: Onset NOAA Scale: G3 or greater Potential Impacts: Area of impact primarily poleward of 50 degrees Geomagnetic Latitude. Induced Currents - Power system voltage irregularities possible, false alarms may be triggered on some protection devices. Spacecraft - Systems may experience surface charging; increased drag on low Earth-orbit satellites and orientation problems may occur. Navigation - Intermittent satellite navigation (GPS) problems, including loss-of-lock and increased range error may occur. Radio - HF (high frequency) radio may be intermittent. Space Weather Scales |
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| Current Condition and Alerts | |
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Issued: 2026 Mar 22 1205 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Geophysical Alert Message Solar-terrestrial indices for 21 March follow. Solar flux 107 and estimated planetary A-index 44. The estimated planetary K-index at 1200 UTC on 22 March was 6.67. Space weather for the past 24 hours has been strong. Geomagnetic storms reaching the G3 level occurred. Space weather for the next 24 hours is predicted to be strong. Geomagnetic storms reaching the G3 level are expected. Space Weather Scales |
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| Forecast Discussion | |
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Issued: 2026 Mar 22 1230 UTC
Prepared
by the U.S. Dept. of Commerce, NOAA, Space Weather Prediction
Center
Solar Activity .24 hr Summary... Solar activity was at low levels with C-class flare activity observed from Region 4399 (S17E75, Hax/alpha). Region 4397 (N16E20, Axx/alpha) showed signs of decay in its trailing spot. New Regions 4400 (S13W19, Bxo/beta), 4401 (N24E72, Hax/alpha) and 4402 (N14E75, Hax/alpha) were numbered this period. No Earth-directed CMEs were observed in available coronagraph imagery. .Forecast... Solar activity is expected to be very low with a chance for a C-class flares and a slight chance for an M-class flare on days one, two, and three (22 Mar, 23 Mar, 24 Mar). Energetic Particle .24 hr Summary... Electrons greater than 2 MeV at geosynchronous orbit were at normal to moderate levels. The greater than 10 MeV proton flux continued at background levels. .Forecast... The greater than 2 MeV electron flux will likely reach high levels on 22 Mar and remain at high levels through 24 Mar. The greater than 10 MeV proton flux is expected to continue at background values. Solar Wind .24 hr Summary... Solar wind parameters reflected CME influences. Solar wind speed reached a peak of 600 km/s at 22/1000Z. Total IMF reached 38 nT at 21/1532Z. The maximum southward component of Bz reached -27 nT at 20/2105Z. Phi varied between positive and negative sectors. .Forecast... The solar wind environment is expected to remain enhanced through the forecast period. CME effects are expected to begin to wane by early on 22 Mar before an additional disturbance due to recurrent, negative polarity CH HSS influences arrive and continue through 24 Mar. Geospace .24 hr Summary... The geomagnetic field was at mostly unsettled to G1 (Minor) levels before reaching G3 (Strong) levels late in the period. .Forecast... G2 (Moderate) to G3 (Strong) geomagnetic storming is likely on 22 Mar due to waning CME influences and the anticipated onset of CH HSS effects. Isolated periods of G1 (Minor) geomagnetic storming are likely on 23 Mar as CH HSS effects continue. Unsettled to active levels are expected to prevail on 24 Mar. Space Weather Scales |
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| Three Day Forecast | |
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Issued: 2026 Mar 22 1230 UTC
Prepared
by the U.S. Dept. of Commerce, NOAA, Space Weather Prediction
Center
A. NOAA Geomagnetic Activity Observation and Forecast The greatest observed 3 hr Kp over the past 24 hours was 7 (NOAA Scale G3). The greatest expected 3 hr Kp for Mar 22-Mar 24 2026 is 6.67 (NOAA Scale G3). NOAA Kp index breakdown Mar 22-Mar 24 2026 Mar 22 Mar 23 Mar 24 00-03UT 3.67 5.00 (G1) 4.00 03-06UT 4.67 (G1) 5.00 (G1) 3.33 06-09UT 5.00 (G1) 3.67 3.00 09-12UT 6.67 (G3) 2.67 2.33 12-15UT 5.33 (G1) 3.00 2.33 15-18UT 3.67 3.00 2.33 18-21UT 3.67 3.33 2.67 21-00UT 5.00 (G1) 3.67 3.00 Rationale: G2 (Moderate) geomagnetic storming is likely on 22 Mar due to waning CME influences and the anticipated onset of CH HSS effects. Isolated periods of G1 (Minor) geomagnetic storming are likely on 23 Mar as CH HSS effects continue. Unsettled to active levels are expected to prevail on 24 Mar. B. NOAA Solar Radiation Activity Observation and Forecast Solar radiation, as observed by NOAA GOES-18 over the past 24 hours, was below S-scale storm level thresholds. Solar Radiation Storm Forecast for Mar 22-Mar 24 2026 Mar 22 Mar 23 Mar 24 S1 or greater 1% 1% 1% Rationale: No S1 (Minor) or greater solar radiation storms are expected. No significant active region activity favorable for radiation storm production is forecast. C. NOAA Radio Blackout Activity and Forecast No radio blackouts were observed over the past 24 hours. Radio Blackout Forecast for Mar 22-Mar 24 2026 Mar 22 Mar 23 Mar 24 R1-R2 10% 10% 10% R3 or greater 1% 1% 1% Rationale: Solar activity is expected to be very low with a chance for a C-class flares and a slight chance for an M-class flare on days one, two, and three (22 Mar, 23 Mar, 24 Mar). Space Weather Scales |
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| Weekly Highlights and Forecasts | |
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Issued: 2026 Mar 16 0302 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Highlights of Solar and Geomagnetic Activity 09 - 15 March 2026 Solar activity was at low to moderate levels with a total of 37 C-class flares and 2 M-class flares observed. The largest flares of the period were an M1.2 flare on 13/0955 UTC from Region 4384 (N10, L=150, class/area Eho/300 on 03 Mar), a C8.9/1n flare on 13/2023 from Region 4392 (S15, L=017, class/area Cso/170 on 15 Mar), and an M1.0/Sf flare on 15/0939 UTC from Region 4392. The most active region of the period was Region 4381 (N08, L=173, class/area Eao/220 on 03 Mar) which produced a long duration C8.0 flare on 13/1518 UTC in addition to 11 other weak C-class events. No proton events were observed at geosynchronous orbit. The greater than 2 MeV electron flux at geosynchronous orbit reached high levels on 09 - 13 Mar and 15 Mar with a peak flux of 2,940 pfu observed at 12/1545 UTC. Normal to moderate levels were observed on 14 Mar. Geomagnetic field activity ranged from quiet to G2 (Moderate) storm levels throughout the 09-15 Mar period. The week began at quiet to unsettled levels on 09 Mar, with active conditions observed on 10-11 Mar due to the influence of a negative polarity coronal hole high speed stream (CH HSS). Conditions returned to mostly quiet to unsettled levels by 12 Mar. Activity intensified midday on 13 Mar, reaching G1 (Minor) to G2 (Moderate) storm levels following the onset of a positive polarity CH HSS. These storming levels continued through the first half of 14 Mar before waning to unsettled and active levels later in the day. On 15 Mar, the field reached active levels early in the period, followed by a return to quiet and unsettled conditions as positive polarity CH HSS effects gradually diminished. Solar wind parameters reflected the influence of two distinct CH HSS regimes during the period. The week began under the influence of a negative polarity CH HSS, with solar wind speeds initially ranging between 450-500 km/s before gradually declining to ambient levels near 400 km/s by 12 Mar. Total magnetic field (Bt) remained mostly around 6 nT during this interval, while the North-South (Bz) component saw periodic southward deflections to -7 nT. A solar sector boundary crossing (SSBC) occurred early on 13 Mar, indicated by a shift in the phi angle from the towards to away sector. This was immediately followed by the onset of a more powerful positive polarity CH HSS. Solar wind speeds rose sharply from 400 km/s to a peak of 725 km/s on 14 Mar. During this period, Bt reached 13 nT and the Bz component reached a maximum southward deflection of -10 nT. By 15 Mar, solar wind speeds began a slow decline but remained elevated near 600 km/s through the end of the period. Forecast of Solar and Geomagnetic Activity 16 March - 11 April 2026 Solar activity is expected to be at low levels, with a slight chance for M-class (R1-R2/Minor-Moderate) flares throughout the outlook period. Elevated probabilities are related to the flare potential of both currently observed spot groups as well as the potential from returning regions. No proton events are expected at geosynchronous orbit. The greater than 2 MeV electron flux at geosynchronous orbit is expected to be at high levels on 16-20, 22-30 Mar, 04-09, and 11 Apr due to the influence from multiple, recurrent, CH HSSs. The remainder of the outlook period is likely to be at normal to moderate levels. Geomagnetic field activity levels are likely to reach G1 (Minor) geomagnetic storm levels on 22 Mar, 04 Apr, 09 Apr, and 11 Apr due to CH HSS influences. G2 (Moderate) geomagnetic storm levels are likely on 11 Mar and 10 Apr due to CH HSS influences. Unsettled to active levels are likely on 16-18, 20, 23-27, 30-31 Mar and 03 and 05-07 Apr. All elevated levels of geomagnetic activity are associated with the anticipated influence of multiple, recurrent, CH HSSs. The remainder of the outlook period is likely to be at mostly quiet levels. Space Weather Scales |
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| About AIA Images | |
| The Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO) is designed to provide an unprecedented view of the solar corona, taking images that span at least 1.3 solar diameters in multiple wavelengths nearly simultaneously, at a resolution of ~ 1 arcsec and at a cadence of 10 s or better. The primary goal of the AIA Science Investigation is to use these data, together with data from other SDO instruments and from other observatories, to significantly improve our understanding of the physics behind the activity displayed by the Sun's atmosphere, which drives space weather in the heliosphere and in planetary environments. The AIA will produce data required for quantitative studies of the evolving coronal magnetic field, and the plasma that it holds, both in quiescent phases and during flares and eruptions; the AIA science investigation aims to utilize these data in a comprehensive research program to provide new understanding of the observed processes Left Click Image for screen size, Right Click Image and open in new tab for full size. | |
| Daily Image AIA 171 | |
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| Daily Image AIA 171 PFSS Model | |
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| Daily Image AIA 193 | |
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| Daily Image AIA 304 | |
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| Daily Video AIA 171 | |
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| Daily Video AIA 171 PFSS Model | |
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| Daily Video AIA 193 | |
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| Daily Video AIA 304 | |
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| About the HMI Images | |
| (Helioseismic and Magnetic Imager) HMI is an instrument designed to study oscillations and the magnetic field at the solar surface, or photosphere. HMI is one of three instruments on the Solar Dynamics Observatory; together, the suite of instruments observes the Sun nearly continuously and takes a terabyte of data a day. HMI observes the full solar disk at 6173 Å with a resolution of 1 arcsecond. HMI is a successor to the Michelson Doppler Imager on the Solar and Heliospheric Observatory. This is very much how the Sun looks like in the visible range of the spectrum (for example, looking at it using special 'eclipse' glasses: Remember, do not ever look directly at the Sun!). The magnetogram image shows the magnetic field in the solar photosphere, with black and white indicating opposite polarities. Left Click Image for screen size, Right Click Image and open in new tab for full size. | |
| Daily Image HMI Continuum | |
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| Daily Image HMI Magnetogram | |
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| Daily Video HMI Continuum | |
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| Daily Video HMI Magnetogram | |
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| About LASCO Images | |
| LASCO (Large Angle Spectrometric Coronagraph) is able to take images of the solar corona by blocking the light coming directly from the Sun with an occulter disk, creating an artificial eclipse within the instrument itself. The position of the solar disk is indicated in the images by the white circle. The most prominent feature of the corona are usually the coronal streamers, those nearly radial bands that can be seen both in C2 and C3. Occasionally, a coronal mass ejection can be seen being expelled away from the Sun and crossing the fields of view of both coronagraphs. The shadow crossing from the lower left corner to the center of the image is the support for the occulter disk. C2 images show the inner solar corona up to 8.4 million kilometers (5.25 million miles) away from the Sun. C3 images have a larger field of view: They encompass 32 diameters of the Sun. To put this in perspective, the diameter of the images is 45 million kilometers (about 30 million miles) at the distance of the Sun, or half of the diameter of the orbit of Mercury. Many bright stars can be seen behind the Sun. Left Click Image for screen size, Right Click Image and open in new tab for full size. | |
| Combined C2 C3 and AIA 304 | |
| NO CURRENT DATA Insert LASCO | |
| Log Polar View C2 C3 and AIA 304 | |
| NO CURRENT DATA Insert Log Polar | |
| Combined C2 C3 and AIA 304 Video | |
| NO CURRENT DATA Insert LASCO Video | |
| Log Polar View C2 C3 and AIA 304 Video | |
| NO CURRENT DATA Insert Log Polar Video | |
| Space Weather Videos | |
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| Space Weather Information | |
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Demystifying Space Weather An article by Scientific Frontline Informative information and glossary about “Space Weather” Space weather has become increasingly important in our modern world due to our growing reliance on technology. It can impact various aspects of our daily lives, from communication and navigation systems to power grids and even astronaut safety. In this deep dive, we'll explore the intricacies of space weather, its causes, its effects, and why understanding it is crucial in our technology-dependent society. |
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