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| Warnings and Alerts | |
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Issue Time: 2026 Mar 25 0826 UTC
ALERT: Geomagnetic K-index of 5 Threshold Reached: 2026 Mar 25 0826 UTC Synoptic Period: 0600-0900 UTC Active Warning: Yes NOAA Scale: G1 - Minor 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 25 1205 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Geophysical Alert Message Solar-terrestrial indices for 24 March follow. Solar flux 128 and estimated planetary A-index 16. The estimated planetary K-index at 1200 UTC on 25 March was 3.67. Space weather for the past 24 hours has been minor. Geomagnetic storms reaching the G1 level occurred. No space weather storms are predicted for the next 24 hours. Space Weather Scales |
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| Forecast Discussion | |
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Issued: 2026 Mar 25 1230 UTC
Prepared
by the U.S. Dept. of Commerce, NOAA, Space Weather Prediction
Center
.24 hr Summary... Solar activity was at low levels, with the largest flare of the period was a C7.2 at 24/1754 UTC from beyond the east limb. A new spot region rotated into few several hours later and was numbered Region 4403 (N16E68, Hax/alpha), though classification is difficult due to substantial foreshortening effects. As Region 4392 (S17, L=16) rotated off the western limb at 24/0000 UTC, there are still seven numbered sunspot groups on the visible disk, with the majority of these regions remaining stable or exhibiting signs of slight decay. Changes were notable in the disks most complex regions: Region 4401 (N25E25, Eai/beta-gamma) has rotated further into view and, alongside significant flux emergence, has revealed a gamma configuration. The trailing spots of Region 4400 (S12W66, Dri/beta) faded throughout the period and simplification around the leading spot led to loss of its delta configuration. An eruption associated with the C7.2 became visible in SOHO LASCO C2 at 24/1800 UTC. While triangulation with STEREO COR2 shows that the CME was not fully farside oriented, modeling indicates no Earth directed component, as the CME was deflected out of the ecliptic plane. A long-duration C3.7 from Region 4400 at 25/0030 UTC also had an associated eruption, first visible in LASCO C2 at 25/0036 UTC. Despite the fast velocity, modeling indicates this eruption is narrow enough that no Earth directed component is expected. .Forecast... Solar activity is expected to be low with a chance for M-class (R1-R2/Minor-Moderate) flares through 27 Mar. Energetic Particle .24 hr Summary... The greater than 2 MeV electron flux at at geosynchronous orbit reached high levels with a peak 11,906 pfu at 24/1605 UTC. The greater than 10 MeV proton flux persisted at nominal background levels with observed minor enhancements likely being the result of high-energy electron contamination in the instrument. .Forecast... The greater than 2 MeV electron flux is expected to continue to reach high levels through 27 Mar. The greater than 10 MeV proton flux is expected to continue at background levels. Solar Wind .24 hr Summary... For the majority of the reporting period, solar wind parameters reflected the continued waning of a negative polarity coronal hole high-speed stream (-CH HSS): wind speed decreasing from ~600 km/s to ~525 km/s; Bt averaging 4 nT with the North-South (Bz) component ranging +/- 4 nT; and the phi angle primarily in a negative (towards the Sun) orientation. At 25/0552 UTC, a magnetic transient began moving through the near-Earth environment, with a slight increase in Bt (3 nT) and more substantial increase in wind speed (~100 km/s). Conditions steadily increased, with Bt reaching a max of 10 nT at 25/0835 nT, and Bz having several southward deflections of sustained -5-7 nT, though the wind speed maintaining an average of approximately 680 km/s. By the end of the reporting period, conditions had begun a gradual decline. .Forecast... Mildly enhanced solar wind parameters are expected to persist through 26 Mar as -CH HSS conditions continue to wane. By late on 26 Mar, additional enhancements are possible as a CME, which departed the Sun on 22 Mar, is forecast to pass in close proximity to Earth. A slow recovery toward nominal levels is anticipated on 27 Mar. Geospace .24 hr Summary... The geomagnetic field reached G1 (Minor) storming levels in the later half of the reporting period due to effects from a magnetic transient. .Forecast... The geomagnetic field is expected to be at unsettled to active levels, with isolated G1 (Minor) storming levels possible, through the rest of 25 Mar as negative polarity CH HSS and the magnetic transient influences gradually diminish. The potential glancing impacts from the 22 Mar CME are expected to result in unsettled to active levels late on 26 Mar. Activity levels are expected to stabilize at quiet to unsettled levels on 27 Mar as transient and coronal hole influences subside. Space Weather Scales |
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| Three Day Forecast | |
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Issued: 2026 Mar 25 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 5 (NOAA Scale G1). The greatest expected 3 hr Kp for Mar 25-Mar 27 2026 is 5.33 (NOAA Scale G1). NOAA Kp index breakdown Mar 25-Mar 27 2026 Mar 25 Mar 26 Mar 27 00-03UT 3.00 3.00 2.33 03-06UT 3.33 2.00 2.67 06-09UT 5.33 (G1) 2.00 2.00 09-12UT 3.67 2.67 2.00 12-15UT 3.67 2.67 1.67 15-18UT 2.00 3.00 2.00 18-21UT 2.67 3.67 2.00 21-00UT 3.00 3.67 2.33 Rationale: No additional G1 (Minor) or greater geomagnetic storms are expected. 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 25-Mar 27 2026 Mar 25 Mar 26 Mar 27 S1 or greater 1% 1% 1% Rationale: No S1 (Minor) or greater solar radiation storms are expected. C. NOAA Radio Blackout Activity and Forecast No radio blackouts were observed over the past 24 hours. Radio Blackout Forecast for Mar 25-Mar 27 2026 Mar 25 Mar 26 Mar 27 R1-R2 25% 25% 25% R3 or greater 5% 5% 5% Rationale: There is a chance for R1-R2 (Minor-Moderate) radio blackouts, with a slight chance for R3 (Strong) events, through 27 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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