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| Warnings and Alerts | |
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Issue Time: 2026 Apr 05 0507 UTC
CONTINUED ALERT: Electron 2MeV Integral Flux exceeded 1000pfu Continuation of Serial Number: 3665 Begin Time: 2026 Apr 03 0920 UTC Yesterday Maximum 2MeV Flux: 2419 pfu Potential Impacts: Satellite systems may experience significant charging resulting in increased risk to satellite systems. Space Weather Scales |
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| Current Condition and Alerts | |
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Issued: 2026 Apr 05 1205 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Geophysical Alert Message Solar-terrestrial indices for 04 April follow. Solar flux 128 and estimated planetary A-index 16. The estimated planetary K-index at 1200 UTC on 05 April was 3.00. Space weather for the past 24 hours has been minor. Radio blackouts reaching the R1 level occurred. Space weather for the next 24 hours is predicted to be moderate. Radio blackouts reaching the R2 level are likely. Space Weather Scales |
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| Forecast Discussion | |
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Issued: 2026 Apr 05 1230 UTC
Prepared
by the U.S. Dept. of Commerce, NOAA, Space Weather Prediction
Center
Solar Activity .24 hr Summary... Solar activity reached moderate levels. Region 4409 (N02W21, Eai/beta-gamma) produced an M1.2/1f flare (R1-Minor) at 04/1211 UTC and an M1.0 flare (R1) at 04/2304 UTC, in addition to numerous C-class flares throughout the period. The region exhibited minor decay and separation among its leader spots. New Region 4412 (N08E15, Bxo/beta) was numbered and produced a few low-level C-flares late in the period. The remaining spotted regions on the visible disk were either mostly stable or in gradual decay. No Earth-directed CMEs were observed in available coronagraph imagery. .Forecast... Solar activity is likely to reach moderate (R1-R2/Minor-Moderate) levels, with a slight chance for X-class (R3/Strong) flares, over 05-07 Apr, driven primarily by the flare potential of Region 4409. Energetic Particle .24 hr Summary... The greater than 2 MeV electron flux reached high levels with a peak flux of 2,420 pfu at 04/1600 UTC. The greater than 10 MeV proton flux continued a gradual decline towards background levels throughout the period. .Forecast... The greater than 2 MeV electron flux is expected to reach high levels on 05-07 Apr. There is a slight chance for the greater than 10 MeV proton flux to exceed S1 (Minor) solar radiation storm levels over 05-07 Apr. Solar Wind .24 hr Summary... Solar wind parameters suggested the return of influence from a negative polarity CH HSS. Total magnetic field strength was steady at around 5 nT and no significant periods of southward Bz were observed. Wind speeds gradually declined from ~650 km/s to between 550-600 km/s by the end of the period. Phi angle was predominantly oriented in the negative solar sector. .Forecast... The solar wind environment is expected to remain enhanced through 07 Apr due to waning negative polarity CH HSS influence. Geospace .24 hr Summary... The geomagnetic field reached active levels during the period under negative polarity CH HSS influences. .Forecast... The geomagnetic field is expected to reach active levels early on 05 Apr, with quiet to unsettled levels expected on 06-07 Apr, as negative polarity CH HSS influences gradually wane. Space Weather Scales |
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| Three Day Forecast | |
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Issued: 2026 Apr 05 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 Apr 05-Apr 07 2026 is 3.67 (below NOAA Scale levels). NOAA Kp index breakdown Apr 05-Apr 07 2026 Apr 05 Apr 06 Apr 07 00-03UT 3.67 2.67 2.67 03-06UT 3.00 3.00 2.67 06-09UT 3.00 2.67 2.67 09-12UT 3.00 2.67 2.00 12-15UT 2.00 2.00 0.67 15-18UT 1.67 1.67 0.67 18-21UT 1.67 1.67 1.67 21-00UT 2.00 2.67 2.67 Rationale: No G1 (Minor) or greater geomagnetic storms are expected. No significant transient or recurrent solar wind features are forecast. 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 Apr 05-Apr 07 2026 Apr 05 Apr 06 Apr 07 S1 or greater 20% 20% 20% Rationale: There is a slight chance for the greater than 10 MeV proton flux to exceed S1 (Minor) solar radiation storm levels over 05-07 Apr. C. NOAA Radio Blackout Activity and Forecast Radio blackouts reaching the R1 levels were observed over the past 24 hours. The largest was at Apr 04 2026 2304 UTC. Radio Blackout Forecast for Apr 05-Apr 07 2026 Apr 05 Apr 06 Apr 07 R1-R2 55% 55% 55% R3 or greater 20% 20% 20% Rationale: R1-R2 (Minor-Moderate) radio blackouts are likely, with a slight chance for X-class R3 (Strong) events, over 05-07 Apr, driven primarily by the flare potential of Region 4409. Space Weather Scales |
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| Weekly Highlights and Forecasts | |
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Issued: 2026 Mar 30 0230 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Highlights of Solar and Geomagnetic Activity 23 - 29 March 2026 Solar activity reached moderate levels on 26 and 28 Mar with low levels observed on 23-25, 27, and 29 Mar. Region 4405 (N26, L=178, class/area=Ehi/330 on 28 Mar) was the most active of the period, producing nine C-class flares and a long-duration M1.3 flare at 28/0416 UTC that was accompanied by a Type II radio sweep (estimated velocity 868 km/s) and a CME first seen in LASCO C2 imagery at 28/0336 UTC. Region 4403 (N16, L=206, class/area=Hsx/120 on 28 Mar) was responsible for the most powerful event of the period, an M3.9/1n flare at 26/0623 UTC, which was associated with a Type II radio sweep (estimated velocity 607 km/s), a 1,600 sfu radio burst at 245 MHz, and a CME first visible in LASCO C2 imagery at 26/0648 UTC. Neither CME was determined to have an Earth-directed component. No proton events were observed at geosynchronous orbit. The greater than 2 MeV electron flux at geosynchronous orbit reached high levels throughout the period 23-29 Mar with peak of 12,800 pfu observed at 27/1515 UTC. Geomagnetic field activity ranged from quiet to G1 (Minor) storm levels. G1 storm conditions were observed 23 Mar due to negative polarity coronal hole high speed stream (-CH HSS) influences. Active levels were observed on 24 Mar under the continuing -CH HSS. On 25 Mar, G1 storming levels were reached again; while residual -CH HSS effects were present, the activity was primarily driven by the arrival of a CME likely associated with a filament eruption on 22 Mar. Conditions waned to unsettled levels on 26 Mar and quiet levels on 27 Mar as HSS influences subsided. Activity remained quiet to unsettled on 28 Mar. On 29 Mar, the field returned to active levels preceding a solar sector boundary crossing (SSBC) and the onset of a positive polarity CH HSS (+CH HSS). Forecast of Solar and Geomagnetic Activity 30 March - 25 April 2026 Solar activity is expected to be is expected to be at low levels, with a varying chance for M-class (R1-R2/Minor-Moderate) flares through 25 Apr. No proton events are expected at geosynchronous orbit, barring any significant, non-recurrent solar activity. The greater than 2 MeV electron flux at geosynchronous orbit is expected to reach high levels on 30-31 Mar, 04-09 Apr, 11-16 Apr, and 18-25 Apr. Normal to moderate flux levels are expected to prevail throughout the remainder of the period. Geomagnetic field activity is expected to reach G1 (Minor) geomagnetic storm levels on 30 March due to the influence of a positive polarity CH HSS (+CH HSS). Periods of G1 storming are likely on 04 April in response to a negative polarity CH HSS (-CH HSS). Further G1 storm periods are anticipated on 09 and 11 Apr, with likely G2 (Moderate) storm levels on 10 April, due to + CH HSS influences. The field is expected to reach G2 storm levels again on 18 Apr, followed by G1 storm periods on 19 Apr, due to -CH HSS influences. Unsettled to active conditions are likely during the onset and waning phases of these streams. 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 | |
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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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