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| Warnings and Alerts | |
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Issue Time: 2026 Mar 28 1632 UTC
WATCH: Geomagnetic Storm Category G1 Predicted Highest Storm Level Predicted by Day: Mar 29: None (Below G1) Mar 30: G1 (Minor) Mar 31: None (Below G1) THIS SUPERSEDES ANY/ALL PRIOR WATCHES IN EFFECT Comment: Isolated periods of G1 (Minor) geomagnetic storming are likely on 30 Mar due to CH HSS effects. Potential Impacts: Area of impact primarily poleward of 60 degrees Geomagnetic Latitude. Induced Currents - Weak power grid fluctuations can occur. Spacecraft - Minor impact on satellite operations possible. Aurora - Aurora may be visible at high latitudes, i.e., northern tier of the U.S. such as northern Michigan and Maine. Space Weather Scales |
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| Current Condition and Alerts | |
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Issued: 2026 Mar 29 1205 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Geophysical Alert Message Solar-terrestrial indices for 28 March follow. Solar flux 162 and estimated planetary A-index 10. The estimated planetary K-index at 1200 UTC on 29 March was 2.33. No space weather storms were observed for the past 24 hours. Space weather for the next 24 hours is predicted to be minor. Geomagnetic storms reaching the G1 level are likely. Space Weather Scales |
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| Forecast Discussion | |
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Issued: 2026 Mar 29 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 due to weak C-class flare activity from Regions 4401 (N25W20, Eai/beta), 4404 (N14E39, Hsx/alpha) and 4405 (S27E52, Eao/beta-gamma). New Region 4408 (N09E72, Hsx/alpha) was numbered this period. No significant changes were noticed in the spotted regions. No Earth-directed CMEs were observed in available coronagraph imagery. .Forecast... Solar activity is expected to be low with a high chance (50%) for M-class flares (R1-R2/Minor-Moderate radio blackouts) through 31 Mar. Energetic Particle .24 hr Summary... Electrons greater than 2 MeV at geosynchronous orbit reached a peak level of 1,600 pfu at 28/1900 UTC. The greater than 10 MeV proton flux remained at background levels. .Forecast... The greater than 2 MeV electron flux is expected to continue to reach high levels through 29 Mar before returning to normal to moderate levels on 30-31 Mar. The greater than 10 MeV proton flux is expected to continue at background levels. Solar Wind .24 hr Summary... Solar wind parameters reflected a mostly nominal regime until approximately 28/2020 UTC when a weak enhancement in the IMF began. Total field increased to 7 nT and the Bz component underwent a southward deflection reaching -7 nT. Solar wind speeds were primarily under 400 km/s. Phi was predominantly in a negative solar sector, but became variable post enhancement. .Forecast... Enhancements from recurrent, positive polarity CH HSS influences are anticipated to begin by late 29 Mar and persist through 30 Mar. Geospace .24 hr Summary... The geomagnetic field was at quiet to active levels. .Forecast... Quiet to active levels are expected on 29 Mar. G1 (Minor) geomagnetic storming is likely on 30 Mar due to recurrent positive polarity CH HSS effects. Unsettled to active conditions are then expected to persist into 31 Mar. Space Weather Scales |
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| Three Day Forecast | |
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Issued: 2026 Mar 29 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 4 (below NOAA Scale levels). The greatest expected 3 hr Kp for Mar 29-Mar 31 2026 is 4.67 (NOAA Scale G1). NOAA Kp index breakdown Mar 29-Mar 31 2026 Mar 29 Mar 30 Mar 31 00-03UT 3.67 3.67 3.67 03-06UT 3.67 4.67 (G1) 3.00 06-09UT 3.33 3.00 2.67 09-12UT 2.33 2.33 2.00 12-15UT 1.67 2.33 2.00 15-18UT 1.67 2.33 2.33 18-21UT 0.67 3.00 2.67 21-00UT 1.00 3.67 2.67 Rationale: G1 (Minor) geomagnetic storming is likely on 30 Mar in response to +CH HSS influences. 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 29-Mar 31 2026 Mar 29 Mar 30 Mar 31 S1 or greater 5% 5% 5% 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 29-Mar 31 2026 Mar 29 Mar 30 Mar 31 R1-R2 50% 50% 50% R3 or greater 10% 10% 10% Rationale: There is a chance for R1-R2 (Minor-Moderate) radio blackouts, and a slight chance for an R3 (Strong) event, on 29-31 Mar. Space Weather Scales |
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| Weekly Highlights and Forecasts | |
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Issued: 2026 Mar 23 0245 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Highlights of Solar and Geomagnetic Activity 16 - 22 March 2026 Solar activity reached moderate levels on 16-18 Mar, with low levels observed on 19-22 Mar. Region 4392 (S16, L=018, class/area=Csi/200 on 17 Mar) produced most of the flare activity observed throughout the week, including three M-flares (R1-Minor). AR4392 produced an M2.7 flare at 16/1215 UTC with accompanying Type-II (est. 1,227 km/s), Type-IV, and Tenflare (380 sfu) emissions. The subsequent asymmetric halo CME, first observed in LASCO C2 imagery at 16/1236 UTC, arrived at Earth on 20 Mar. AR4392 produced another M2.7 flare at 18/0842 UTC with accompanying Type-II (est. 860 km/s) and Tenflare (229 sfu) emissions. The associated CME, first visible in LASCO C2 imagery at 18/0936 UTC, arrived simultaneously with the 16 Mar CME on 20 Mar. No proton events were observed at geosynchronous orbit. The greater than 2 MeV electron flux at geosynchronous orbit reached high levels on 16-20 and 22 Mar. Normal to moderate levels were observed on 21 Mar following a period of elevated geomagnetic field activity. Geomagnetic field activity reached G1-G3 (Minor-Strong) geomagnetic storm levels on 20-22 Mar, following the arrival of multiple CMEs (that left the Sun on 16 and 18 Mar) on 20 Mar. The remainder of the period was at quiet and quiet to unsettled levels under ambient solar wind conditions. Forecast of Solar and Geomagnetic Activity 23 March - 18 April 2026 Solar activity is expected to be at low levels with a varying chance for M-class (R1-R2/Minor-Moderate) flares through 18 Apr. No proton events are expected at geosynchronous orbit, barring significant flare activity. The greater than 2 MeV electron flux at geosynchronous orbit is expected to reach high levels on 23-25, 27-28, 30-31 Mar and 04-09, 11-15 Apr. Normal to moderate flux levels are expected to prevail throughout the remainder of the period. Geomagnetic field activity is expected to reach G1-G2 (Minor-Moderate) geomagnetic storm levels on 23 Mar due to negative polarity CH HSS influences. Periods of G1 (Minor) storming are likely on 03-04 Apr in response to negative polarity CH HSS influences. Periods of G1 (Minor) storming are likely on 09 and 11 Apr, with G2 (Moderate) storm periods likely on 10 Apr, due to positive polarity CH HSS influences. G2 (Moderate) storm periods are likely again on 18 Apr following the onset of negative polarity CH HSS influences. 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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