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| Warnings and Alerts | |
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Issue Time: 2026 Mar 03 2305 UTC
WATCH: Geomagnetic Storm Category G1 Predicted Highest Storm Level Predicted by Day: Mar 04: None (Below G1) Mar 05: None (Below G1) Mar 06: G1 (Minor) THIS SUPERSEDES ANY/ALL PRIOR WATCHES IN EFFECT 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 06 1205 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Geophysical Alert Message Solar-terrestrial indices for 05 March follow. Solar flux 146 and estimated planetary A-index 4. The estimated planetary K-index at 1200 UTC on 06 March was 1.67. 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 06 1230 UTC
Prepared
by the U.S. Dept. of Commerce, NOAA, Space Weather Prediction
Center
Solar Activity .24 hr Summary... Solar activity continued at low levels. Predominently B-class, with isolated C-class, flares were observed. Region 4381 (N08W12, Dai/beta) exhibited moderate growth in its intermediate and trailing spots, and kicked off a C1.8 flare at 05/1950 UTC. New Region 4386 (N16W70, Bxo/beta) was numbered, and was the only other spot group to experience growth during the period. The remaining numbered regions were mostly unchanged and inactive. Additional activity included a filament eruption in the SE quadrant, centered near S20E30. A CME was noted in C2 coronagraph imagery starting at 06/0428 UTC. Modeling efforts are underway at the time of this summary. .Forecast... Solar activity is expected to be at low levels, with a slight chance for isolated M-class activity (R1-R2/Minor-Moderate) through 08 Mar. Energetic Particle .24 hr Summary... The greater than 2 MeV electron flux was at moderate levels with a peak of 581 pfu observed at 05/1440 UTC. The greater than 10 MeV proton flux remained at background levels. .Forecast... The greater than 2 MeV electron flux is to remain at moderate levels 06 Mar before reaching high levels on 07-08 Mar. The greater than 10 MeV proton flux is expected to continue at background levels through 08 Mar. Solar Wind .24 hr Summary... Solar wind parameters were indicative of a near-backgroud solar wind regime. A slight enhancement was observed near 06/0400 UTC, however, parameters remained at near nominal levels. Solar wind speed was between 350-400 km/s. Aside from a brief increase to 10 nT, total magnetic field (Bt) averaged around 5 nT, the North-South (Bz) component was variable between +/-5 nT, and the Phi angle switched from positive to negative towards the end of the period. .Forecast... Solar wind conditions are expected to continue near ambient levels for the first half of 06 Mar. By late on 06 Mar to early on 07 Mar, the onset of a stronger negative polarity coronal hole high-speed stream (-CH HSS) is anticipated. Geospace .24 hr Summary... The geomagnetic field was at quiet to unsettled levels. .Forecast... The geomagnetic field is expected to be at mostly quiet levels early on 06 Mar as lingering enhancements subside; G1 (Minor) storming is likely later on 06 Mar due to the anticipated onset of a negative polarity coronal hole high-speed stream (-CH HSS). Active conditions are expected 07-08 Mar as high-speed stream influences continue. Space Weather Scales |
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| Three Day Forecast | |
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Issued: 2026 Mar 06 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 3 (below NOAA Scale levels). The greatest expected 3 hr Kp for Mar 06-Mar 08 2026 is 4.67 (NOAA Scale G1). NOAA Kp index breakdown Mar 06-Mar 08 2026 Mar 06 Mar 07 Mar 08 00-03UT 1.00 3.67 4.00 03-06UT 2.67 3.33 2.00 06-09UT 1.67 2.00 2.00 09-12UT 1.67 1.67 2.00 12-15UT 3.67 3.00 2.67 15-18UT 4.00 3.33 2.67 18-21UT 4.67 (G1) 3.67 2.67 21-00UT 4.33 3.33 3.00 Rationale: Isolated G1 (Minor) geomagnetic storms are possible on 06 Mar due to the anticipated arrival of a CIR associated with a negative polarity coronal hole high speed stream. 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 06-Mar 08 2026 Mar 06 Mar 07 Mar 08 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 06-Mar 08 2026 Mar 06 Mar 07 Mar 08 R1-R2 20% 20% 20% R3 or greater 1% 1% 1% Rationale: There is a slight chance for R1-R2 (Minor-Moderate) radio blackouts through 08 Mar. Space Weather Scales |
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| Weekly Highlights and Forecasts | |
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Issued: 2026 Mar 02 0144 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Highlights of Solar and Geomagnetic Activity 23 February - 01 March 2026 Solar activity was reached moderate after an M2.3 flare at 25/1154 UTC from Region 4379 (S17, L=205, class/area=Bxo/050 on 26 Feb). A Type II radio sweep was also observed on 25 Feb, associated with a 5-degree filament eruption near S08W27 and a C2.6 flare at 25/0656 UTC. Modeling of the ejecta from the event suggested possible glancing influence at Earth on 28 Feb - 01 Mar. For the remainder of the week, activity was observed between low and very low levels. No proton events were observed at geosynchronous orbit. The greater than 2 MeV electron flux at geosynchronous orbit was primarily at high levels through the past seven days. Geomagnetic field activity was reached G1 (Minor) geomagnetic storm levels on 23 Feb during the onset of a negative polarity CH HSS. Solar wind speeds increased from ~450 km/s to ~700 km/s. Total magnetic field strength peaked around 7 nT, then fell to at or below 5 nT for the remainder of the outlook period. Active conditions were observed over 24-26 Feb and finally to unsettled levels over 27 Feb - 01 Mar as solar wind speeds from the coronal hole gradually waned. Forecast of Solar and Geomagnetic Activity 02 March - 28 March 2026 Solar activity is expected to be at low levels, with a change 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 on the visible disk as well as the potential from regions that are expected to return from the Sun's farside. No proton events are expected at geosynchronous orbit. The greater than 2 MeV electron flux at geosynchronous orbit is expected to reach high levels on 02-08 Mar, 11-12 Mar, 15-19 Mar, and 21-28 Mar due to anticipated influence from multiple, recurrent, CH HSSs. The remainder of the outlook period is likely to be at normal to moderate levels. Geomagnetic field activity is expected to range from quiet to G2 (Moderate) geomagnetic storm levels. G2 conditions are likely on 21 Mar; G1 (Minor) conditions are likely on 22 Mar; active conditions are likely on 03 Mar, 10 Mar, 12 Mar, 14-15 Mar, 20 Mar, and 23-25 Mar; unsettled conditions are likely on 02 Mar, 04 Mar, 06 Mar, 08-09 Mar, 11 Mar, 13 Mar, 16-19 Mar, and 26-28 Mar. 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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| 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 | |
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| Log Polar View C2 C3 and AIA 304 | |
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| Combined C2 C3 and AIA 304 Video | |
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| Log Polar View C2 C3 and AIA 304 Video | |
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| 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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