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| Warnings and Alerts | |
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Issue Time: 2026 Apr 09 0459 UTC
CONTINUED ALERT: Electron 2MeV Integral Flux exceeded 1000pfu Continuation of Serial Number: 3669 Begin Time: 2026 Apr 03 0920 UTC Yesterday Maximum 2MeV Flux: 7322 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 09 1205 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Geophysical Alert Message Solar-terrestrial indices for 08 April follow. Solar flux 108 and estimated planetary A-index 7. The estimated planetary K-index at 1200 UTC on 09 April was 1.33. 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 minor. Geomagnetic storms reaching the G1 level are likely. Space Weather Scales |
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| Forecast Discussion | |
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Issued: 2026 Apr 09 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. While much of the period was characterized by periodic B- and C-class flaring, Region 4409 (N01W78, Esi/beta-delta) produced an M1.0/Sf flare at 09/0845 UTC. Additionally, Region 4414 (N15E43, Dro/beta) was responsible for a C8.7/Sf flare at 08/1543 UTC. There are currently six numbered active regions on the visible disk. Region 4409 remains the most complex group on the disk, appearing relatively static with some evidence of decline in its intermediary spots, though a definitive assessment of its magnetic configuration is increasingly hindered by western limb proximity. Region 4413 (N07W83, Dac/beta) appeared to undergo significant magnetic simplification with a corresponding decay in extent, though extreme limb proximity makes this too difficult to confirm. The development of Region 4414 was mixed with new flux emergence around the leading spots while the trailing spots showed significant decay. The remaining regions remained largely stable throughout the period. Coronal activity was complex and difficult to characterize in available imagery. An eruption to the East was observed in LASCO C2 at 08/1648 UTC, potentially associated with the C8.7 flare from Region 4414. This feature appeared as a subtle, second shock front silhouetted against a prior eruption first seen at 08/0536 UTC. Confidence in this second eruption is low due to its faint signature and the visual interference of the preceding event. Furthermore, the feature is not discernible in STEREO A COR2 imagery, suggesting that if an eruption occurred, it is likely directed far to the east of the Sun-Earth line. Modeling of the suspected source region indicates no Earth-directed component. .Forecast... Solar activity is expected to be at low levels 09-11 Apr with a chance for M-class (R1-R2/Minor-Moderate) flares. A slight chance for X-class (R3/Strong and above) flaring exists 09 Apr until diminishing as Region 4409 rotates off the visible disk. Energetic Particle .24 hr Summary... The greater than 2 MeV electron flux was at high levels with a peak flux of 7,322 pfu at 08/1555 UTC. The greater than 10 MeV proton flux was at background levels. .Forecast... The greater than 2 MeV electron flux is expected to continue to reach high levels through 09 Apr. A drop to moderate levels is forecasted for 10 Apr due to the anticipated arrival of a corotating interacting region (CIR) before again reaching high levels on 12 Apr due to the onset of a positive polarity coronal hole high speed stream (+CH HSS). The greater than 10 MeV proton flux is expected to remain at background levels. Solar Wind .24 hr Summary... Solar wind parameters reflected near-nominal, quiet-regime conditions throughout the reporting period. Wind speeds averaged approximately 375 km/s and gradually declined throughout the period. The total magnetic field (Bt) averaged around 5 nT, while the North-South (Bz) component was predominantly southward and reached a maximum deflection of -4 nT. The phi angle exhibited a three-hour excursion into the positive (away) sector mid-period, though it remained predominantly in a negative (towards) orientation. .Forecast... Solar wind parameters are expected to remain at nominal conditions through 09 Apr. Disturbed conditions are anticipated on 10 Apr, followed by elevated parameters on 11 Apr, due to the arrival of a CIR and the subsequent onset of a +CH HSS. Geospace .24 hr Summary... The geomagnetic field was at quiet levels. .Forecast... The geomagnetic field is expected to remain mostly quiet 09 Apr. G1 (Minor) storming levels are anticipated 10-11 Apr due to the arrival of the CIR and the effects of the +CH HSS.. Space Weather Scales |
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| Three Day Forecast | |
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Issued: 2026 Apr 09 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 2 (below NOAA Scale levels). The greatest expected 3 hr Kp for Apr 09-Apr 11 2026 is 5.33 (NOAA Scale G1). NOAA Kp index breakdown Apr 09-Apr 11 2026 Apr 09 Apr 10 Apr 11 00-03UT 1.67 2.33 5.33 (G1) 03-06UT 1.00 5.00 (G1) 4.00 06-09UT 2.00 4.33 4.00 09-12UT 1.33 3.67 3.33 12-15UT 2.00 2.67 3.67 15-18UT 1.67 2.67 4.00 18-21UT 1.67 3.67 4.67 (G1) 21-00UT 1.67 4.33 4.67 (G1) Rationale: G1 (Minor) or greater geomagnetic storms are likely on 10 and 11 Apr due to positive polarity coronal hole high speed stream onset. 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 09-Apr 11 2026 Apr 09 Apr 10 Apr 11 S1 or greater 10% 5% 1% Rationale: There is a slight and declining chance for the greater than 10 MeV proton flux to exceed S1 (Minor) solar radiation storm level 09-11 Apr primarily due to the complexity of Region 4409 and its forthcoming rotation off the visible disk. 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 09 2026 0845 UTC. Radio Blackout Forecast for Apr 09-Apr 11 2026 Apr 09 Apr 10 Apr 11 R1-R2 30% 20% 20% R3 or greater 10% 5% 1% Rationale: There is a chance for R1-R2 (Minor-Moderate) radio blackouts on 09 Apr with a slight chance for R1-R2 (Minor-Moderate) radio blackouts 10-11 Apr and for R3 (Strong) or greater events through 11 Apr primarily due to the development of Regions 4409 and 4414. Space Weather Scales |
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| Weekly Highlights and Forecasts | |
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Issued: 2026 Apr 06 0211 UTC
Prepared
by the US Dept. of Commerce, NOAA, Space Weather Prediction
Center
Highlights of Solar and Geomagnetic Activity 30 March - 05 April 2026 Solar activity reached high levels on 30 Mar and 04 Apr, moderate levels on 02-03 Apr, with low levels observed on 31 Mar, 01 Apr, and 5 Apr. Region 4409 (N02, L=156, class/area=Eai/170 on 04 Apr) was the most active of the period, producing 50 C-class flares and six M-class flares. Region 4405 (S27, L=220, class/area=Eai/220 on 02 Apr) added the strongest flare of the period, an X1.4/Sf flare, on 30 Mar at 0319 UTC. Accompanying the flare was a Type II radio sweep (estimated velocity 1872 km/s) and a partial halo CME first seen in LASCO C2 imagery at 30/0312 UTC. Expected impacts from this CME were on 01 Apr. Region 4409 also produced a C8.1 flare at 01/1958 UTC. Accompanying this flare was a filament eruption and subsequent CME that had a likely Earth-directed trajectory with impacts likely felt on 03-04 Apr. Slightly elevated proton levels were observed from 01-05 Apr, but conditions remained below alert thresholds throughout the period. The greater than 2 MeV electron flux at geosynchronous orbit reached high levels throughout most of the period of 30 Mar - 05 Apr, with a peak flux value of 6,000 pfu observed at 05/1645 UTC. The only exception was on 02 Apr when conditions dropped to moderate levels for that 24 hour reporting period. Geomagnetic field activity ranged from quiet to G3 (Strong) storm levels during the 30 Mar - 05 Apr period. Quiet to unsettled levels were observed on 30 Mar - 01 Apr, and most of 05 Apr (aside from an isolated active period at the beginning of the UT day). Conditions increased to active to G2 (Moderate) levels on 02 Apr following the onset of a negative polarity coronal hole high speed stream (CH HSS). Conditions remained at active to G1 (Minor) levels through midday on 03 Apr when they increased to G3 (Strong) levels with the arrival of the anticipated CME from 01 Apr (C8.1 flare and filament eruption). Conditions then decreased to G1 levels to start 04 Apr, before decreasing to quiet to active conditions lasting through 05 Apr. Forecast of Solar and Geomagnetic Activity 06 April - 02 May 2026 Solar activity is expected to be at low levels, with a varying chance for M-class (R1-R2/Minor-Moderate) flares, and a slight chance for X-Class (R3/Strong) flares from 06 Apr through 02 May. 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 06-09 Apr, 11-16 Apr, and 18 Apr-02 May. Normal to moderate flux levels are expected on 10 and 17 Apr. Geomagnetic field activity is anticipated to reach G1/G2 (Minor/Moderate) geomagnetic storm levels on 18-19, and 29 Apr due to the influence of negative polarity CH HSS (-CH HSS). Periods of G1 (Minor) storming are likely on 04 April in response to a negative polarity CH HSS (-CH HSS). Unsettled to Active levels are expected on 06-07 Apr, 20-22 Apr, and 30 Apr, as well as 01-02 May associated with negative polarity CH HSS effects. On 10-13 and 25-26 April, positive polarity CH HSS influences are expected to bump geomagnetic conditions to unsettled to active levels. Mostly quiet levels are expected during all other days of the period. 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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